List of largest exoplanets

Below is a list of the largest exoplanets so far discovered, in terms of physical size, ordered by radius.

Jupiter as seen by Voyager 1 in 1979. It is the largest planet having its surface resolved^[1][2][3] and it is the largest planet in the Solar System.^[4]

Limitations

This list of extrasolar objects may and will change over time due to diverging measurements published between scientific journals, varying methods used to examine these objects, and the notably difficult task of discovering extrasolar objects in general. These objects are not stars, and are quite small on a universal or even stellar scale. Furthermore, these objects might be brown dwarfs, sub-brown dwarfs, or not even exist at all. Because of this, this list only cites the most certain measurements to date and is prone to change.

List

This is a dynamic list and may never be able to satisfy particular standards for completeness. You can help by adding missing items with reliable sources.

The sizes are listed in units of Jupiter radii (R_J, 71 492 km). This list is designed to include all exoplanets that are larger than 1.6 times the size of Jupiter. Some well-known exoplanets that are smaller than 1.6 R_J (17.93 R_🜨 or 114387.2 km) have been included for the sake of comparison.

Key (Classification)

*	Probably brown dwarfs (≳ 13 MJ) (based on mass)
†	Probably sub-brown dwarfs (based on mass and location)
?	Uncertain status (inconsistency in age or mass of planetary system)
!	Uncertain status while probably brown dwarfs (≳ 13 MJ) (based on mass)
←	Probably exoplanets (≲ 13 MJ) (based on mass)
→	Planets with grazing transit, hindering radius determination
#	Notable non-exoplanets reported for reference
–	Theoretical planet size restrictions

Key (Illustration)

	Artist's impression
	Artist's size comparison
	Artist's impression size comparison
	Direct imaging telescopic observation
	Direct image size comparison
	Composite image of direct observations
	Transiting telescopic observation
	Simulation observation

Illustration	Name (Alternates)	Radius (RJ)	Key	Mass (MJ)	Notes
	Sun (Sol)	9.731 (1 R☉)[5] (695 700 km)[a]	#	1047.569 (1 M☉)[5] (1.988 416 × 1030 kg)[b]	The only star in the Solar System. Responsible for life on Earth and keeping the planets on orbit. Age: 4.6 Gyr.[10] Reported for reference.
	Toliman (Alpha Centauri B)	8.360 ± 0.035[11] (0.8591 ± 0.0036 R☉)	#	952.450 ± 2.619[11] (0.9092 ± 0.0025 M☉)	One of first two stars (other being Rigil Kentaurus / Alpha Centauri A) to have its stellar parallax measured.[12] Nearest binary star system and nearest stellar system to the Sun at the distance of 4.344 ± 0.002 ly (1.33188 ± 0.00061 pc). A member of Alpha Centauri System, the nearest system to the Sun. Age: 5.3 ± 0.3 Gyr.[13] Reported for reference.
	Maximum size of planetary-mass object	8[14]	–	~ 5[14]	Maximum theoretical size limit assumed for a ~ 5 MJ mass object right after formation, however, for 'arbitrary initial conditions'.
	Proplyd 133-353	≲ 7.82 ± 0.81[15][c] (≲ 0.804 ± 0.083 R☉)	†	(≲) 13[15]	A candidate sub-brown dwarf or rogue planet with a photoevaporating disk, located in the Orion Nebula Cluster. At a probable age younger than 500 000 years, it is one of the youngest free-floating planetary-mass candidates known.[15] More information about Proplyd 133-353 and estimates of its radius are available:[h]
	2M0535-05 A (V2384 Orionis A)	6.71 ± 0.11[16] (0.690 ± 0.011 R☉)	#	59.9 ± 3.5[16] (0.0572 ± 0.0033 M☉)	First eclipsing binary brown dwarf system to be discovered, orbiting around 9.8 days.[17][18] Age: ~1 Myr[19] Reported for reference.
	2M0535-05 B (V2384 Orionis B)	5.25 ± 0.09[16] (0.540 ± 0.009 R☉)	#	38.3 ± 2.3[16] (0.0366 ± 0.0022 M☉)
	KPNO-Tau-4	4.1[20][21]	†	10.5[20]	A member of Taurus-Auriga star-forming region.[21]
	GQ Lupi b (GQ Lupi Ab, GQ Lupi B)	3.77[22]	*	20 ± 10;[23] 1 – 46[24]	First confirmed exoplanet candidate to be directly imaged. GQ Lupi b has a mass of 1 – 46 MJ; in the higher half of this range, it may be classified as a young brown dwarf. It should not be confused with the star GQ Lup C (2MASS J15491331), 2400 AU away, sometimes referred to as GQ Lup B.[25] Other sources of the radius include 3.7±0.7 RJ,[26] 3.0±0.5 RJ,[24] 3.5+1.50 −1.03 RJ,[27] 4.6 ± 1.4 RJ, 6.5 ± 2.0 RJ.[28]
	HD 100546 b (KR Muscae b)	3.4[29]	*	25[29]	Sometimes the initially reported 6.9 +2.7 −2.9 RJ for the emitting area due to the diffuse dust and gas envelope or debris disk surrounding the planet[30] is confused with the actual radius. Other source of mass: 1.65 MJ.[31] HD 100546 system is the closest planetary system that contains a Herbig Ae/Be star.[32]
	2MASS J0437+2331	3.30[33][i]	†	7.1 +1.1 −1.0[33]	May be a sub-brown dwarf or a rogue planet
	OTS 44	3.2 – 3.6[34]	†	11.5[35]	First discovered rogue planet; very likely a brown dwarf[36] or sub-brown dwarf.[37] It is surrounded by a circumstellar disk of dust and particles of rock and ice. The currently preferred radius estimate is done by SED modelling including substellar object and disk model.[34]
	2MASS J044144b (2M 0441+23 Bb)	3.06[38][i]	†	9.8 ± 1.8[38]	Based on the mass ratio to 2M J044145 A (2M 0441+23 Aa) it is likely not a planet according to the IAU's exoplanet working definition.[39] Part of the lowest mass quadruple 2M 0441+23 system of 0.26 M☉.[38]
	Kapteyn's Star	2.83 ± 0.24[40] (0.291 ± 0.025 R☉)	#	294.4 ± 14.7[40] (0.2810 ± 0.014 M☉)	The closest halo star and nearest red subdwarf, at the distance of 12.82 ly (3.93 pc), and second-highest proper motion of any stars of more than 8 arcseconds per year (after the Barnard's Star). Age: 11.5 +0.5 −1.5 Gyr.[41] Reported for reference.
	AB Aurigae b (AB Aur b)	< 2.75[42][j]	!	20 (~ 4 Myr),[43] 10 – 12 (1 Myr), < 130[42]	Likely a brown dwarf; Assuming a hot-start evolution model and a planetary mass, AB Aurigae b would be younger than 2 Myr to have its observed large luminosity, which is inconsistent with the age of AB Aurigae of 6.0 +2.5 −1.0 Myr, which could be caused by delayed planet formation in the disk.[44] Other system ages include 1 - 5 Myr,[42] 4 ± 1 Myr[45] and 4 Myr.[46] Another source gives a higher mass of 20 MJ in the brown dwarf regime for an age of 4 Myr, arguing since gravitational instability of the disk (preferred formation mechanism in the discovery publication)[42] operates on very short time scales, the object might be as old as AB Aur.[43] A more recent study also support the latter source, given the apparent magnitude was revised upwards.[47]
	DH Tauri b (DH Tau b)	2.7 ± 0.8[28]	←	11 ± 3[28]	First planet to have a confirmed circumplanetary disk, detected with polarimetry at the VLT[48] and youngest confirmed planet at an age of 0.7 Myr.[26] DH Tauri b is suspected to have an exomoon candidate orbiting it every 320 years, with about the same mass as Jupiter.[49] Other sources give the radii: 2.6±0.6 RJ,[26] 2.49 RJ[34][i] and masses: 14.2 +2.4 −3.5 MJ,[50] 17 ± 6 MJ,[51] 12 ± 4 MJ.[26]
	CT Chamaeleontis b (CT Cha b)	2.6 +1.2 −0.2[34]	*	17 ± 6[52]	Likely a brown dwarf.[53] Furthest planet to be directly imaged at the dstance of 622 ly (190.71 pc).[54]
	CM Draconis A (Gliese 630.1 Aa)	2.4437 ± 0.0002[55] (0.25113 ± 0.00016 R☉)	#	235.8 ± 0.3[55] (0.22507 ± 0.00024 M☉)	Second eclipsing binary red dwarf system discovered after YY Geminorum AB (Castor Cab).[56] One of the lightest stars with precisely measured masses and radii, orbiting around 1.268 days. The members of Gliese 630.1 triple system. Age: 4.1 ± 0.8 Gyr.[57] Reported for reference.
	PZ Telescopii b (PZ Tel b, HD 174429 b)	2.42 +0.28 −0.34[58]	*	27 +25 −9[59]	Likely a brown dwarf. First possible extra Jupiter-like planet to be directly imaged[60]
	CM Draconis B (Gliese 630.1 Ab)	2.3094 ± 0.0001[55] (0.23732 ± 0.00014 R☉)	#	220.2 ± 0.3[55] (0.21017 ± 0.00028 M☉)	Second eclipsing binary red dwarf system discovered after YY Geminorum AB (Castor Cab).[56] One of the lightest stars with precisely measured masses and radii, orbiting around 1.268 days. The members of Gliese 630.1 triple system. Age: 4.1 ± 0.8 Gyr.[57] Reported for reference.
	o005 s41280	2.30[61]	†	8.4[61]	May be a sub-brown dwarf or a rogue planet[61]
	TWA 29	2.222 +0.082 −0.081[62]	†	6.6 +5.2 −2.9[62]	Rogue planet
	Hot Jupiter limit	2.2[63]	–	> 0	Theoretical size limit for hot Jupiters close to a star, that are limited by tidal heating, resulting in 'runaway inflation'
	XO-6b	2.17 ± 0.2[64]	←	4.47 ± 0.12[64]	A very puffy Hot Jupiter
	HAT-P-67b	2.140±0.025[65]	←	0.45±0.15[65]	A very puffy Hot Jupiter. Was the largest known planet with an accurately and precisely measured radius (2.085 +0.096 −0.071 RJ),[66][67] until a new estimate revised its radius in 2024[68][64] and again in 2025.[65]
	PSO J077.1+24	2.14[33][i]	†	5.9 +0.9 −0.8[33]	Rogue planet
	CAHA Tau 1	2.12[69][70][i]	†	10 ± 5[69][70]	Rogue planet
	ROXs 42B b	2.10 ± 0.35[26]	←	9 +6 −3,[71] 10 ± 4[72]	Older estimates include 1.9 – 2.4, 1.3 – 4.7 RJ[73] and 2.43±0.18, 2.55±0.2 RJ.[74] Other recent sources of masses include 3.2 – 27 MJ,[75] 13 ± 5 MJ.[26]
	HATS-15b	2.019 +0.202 −0.160[76]	←	2.17 ± 0.15[76]
	Cha 110913-773444 (Cha 110913)	2.0 – 2.1[34]	†	8 +7 −3[77]	A rogue planet/sub-brown dwarf that is surrounded by a protoplanetary disk, the first one to be confirmed. It is one of youngest free-floating substellar objects with 0.5–10 Myr. The currently preferred radius estimate is done by SED modelling including substellar object and disk model.[34]
	CFHTWIR-Oph 90 (Oph 90)	2.00 +0.09 −0.12;[78] 3[79][80]	†	10.5[79]	May be rogue planet or brown dwarf
	SSTB213 J041757 A	2[81]	†	3.5[81]	In a binary with a smaller 1.7 RJ planet.
	Kepler-435b (KOI-680 b)	1.99 ± 0.18[82]	←	0.84 ± 0.15[82]
	PDS 70 c	1.98 +0.39 −0.31[83]	←	7.5 +4.7 −4.2, 7.8 +5.0 −4.7, ~1 − ~15 (total)[84]	First confirmed directly imaged exoplanet still embedded in the natal gas and dust from which planets form (protoplanetary disk) and the second protoplanet to have a confirmed circumplanetary disk (after DH Tauri b).[85] PDS 70 is the second multi-planet system to be directly imaged (after HR 8799).
	PDS 70 b	1.96 +0.20 −0.17[83]	←	3.2 +3.3 −1.6, 7.9 +4.9 −4.7, < 10 (2 σ), ≲ 15 (total)[84]	First protoplanet to have been ever detected. PDS 70 is the second multiplanetary system to be directly imaged (after HR 8799 system). Other source of radius includes 2.7 RJ.[44]
	OGLE2-TR-L9b	1.958 +0.174 −0.111[76]	←	4.5 ± 1.5}}[76]	First discovered planet orbiting a fast-rotating hot star, OGLE2-TR-L9.[86]
	CFHTWIR-Oph 98 A	1.95 +0.11 −0.10;[78] 2.14[79][87]	*	15.4 ± 0.8;[88] 10.5[79]	Either a M-type brown dwarf or sub-brown dwarf with a sub-brown dwarf/planet companion CFHTWIR-Oph 98 b. Other sources of masses includes: 9.6 – 18.4 MJ.[88]
	WASP-178b (KELT-26 b, HD 134004 b)	1.940 +0.060 −0.058[89]	←	1.41 +0.43 −0.51[89]	An ultra-hot Jupiter. Initially, the planet's atmosphere was discovered having silicon monoxide, making this exoplanet the first one to have the compound on its atmosphere,[90] now the atmosphere is more likely dominated by ionized magnesium and iron.[91]
	WASP-12Ab	1.937 ± 0.056[92]	←	1.47 +0.076 −0.069[93]	This planet is so close to WASP-12 A that its tidal forces are distorting it into an egg-like shape.[94] First planet observed being consumed by its host star;[95] it will be destroyed in 3.16 ± 0.10 Ma due to tidal interactions.[96][97] WASP-12b is suspected to have one exomoon due to a curve of change of shine of the planet observed regular variation of light.[98]
	BD-14 3065 b (TOI-4987 b)	1.926 ± 0.094[99]	*	12.37 ± 0.92[99]	Might be a brown dwarf fusing deuterium at its core, which could explain its anomalous high radius. Also one of the hottest known exoplanets, measuring 3,520 K (3,250 °C; 5,880 °F).[99]
	KELT-9b (HD 195689 b)	1.891 +0.061 −0.055[100]	←	2.17 ± 0.56[101]	Hottest confirmed exoplanet, with a temperature of 4050±180 K (3777 ± 180 °C; 6830 ± 324 °F).[102]
	TOI-1518 b	1.875 ± 0.053[103]	←	< 2.3 (2 σ)[103]
	HAT-P-70b	1.87 +0.15 −0.10[104]	←	< 6.78 (3 σ)[104]
	2MASS J1935-2846	1.869 ± 0.053[105]	†	7.4 +6.3 −3.4[105]	May be a sub-brown dwarf or rogue planet.
	HATS-23b	1.86 +0.30 −0.40[106]	→	1.470 ± 0.072[106]	Grazing planet.
	CFHTWIR-Oph 98 b (Oph 98 b, CFHTWIR-Oph 98 B)	1.86 ± 0.05[54][87]	†	7.8 +0.7 −0.8[88]	Its formation as an exoplanet is challenging or impossible.[107] If its formation scenario is known, it may explain the formation of Planet Nine. Planetary migration may explain its formation, or it may be a sub-brown dwarf. Other sources of mass includes 4.1 – 11.6 MJ.[88]
	KELT-8b	1.86 +0.18 −0.16[108]	←	0.867 +0.065 −0.061[108]
	KPNO-Tau 12	1.84,[20] 2.22 +0.11 −0.17[78]	†	11.5[79]	A member of Taurus-Auriga star-forming region.[20]
	TrES-4 (GSC 06200-00648 Ab)	1.838 +0.240 −0.238[76]	←	0.78 ± 0.19[109]	This planet has a density of 0.17 g/cm3,[76] about that of balsa wood, less than Saturn's 0.7 g/cm3.
	HAT-P-33b	1.827 ± 0.29,[110] 1.85±0.49[54]	←	0.72 +0.13 −0.12[111]
	HAT-P-32b	1.822 +0.350 −0.236[76]	←	0.941 ± 0.166, 0.860 ± 0.164[112]
	KELT-20b (MASCARA-2b)	1.821±0.045[113]	←	3.355+0.062 −0.063[113]	An ultra-hot Jupiter.
	YSES 1 b (TYC 8998-760-1 b)	1.82 ± 0.08[114] – 3.0 +0.2 −0.7[115]	*	21.8 ± 3[116]	Likely a brown dwarf. First substellar object to have an isotope (13C) in its atmosphere.[117][114] First directly imaged planetary system having multiple bodies orbiting a Sun-like star.[118][119]
	Barnard's Star	1.82 ± 0.01[120] (0.187 ± 0.001 R☉)	#	168.7 +3.8 −3.7[120] (0.1610 +0.0036 −0.0035 M☉)	Second nearest planetary system to the Sun at the distance of 5.97 ly (1.83 pc) and closest star in the northern celestial hemisphere. Also the highest proper motion of any stars of 10.3 arcseconds per year relative to the Sun. Has 4 confirmed planet, Barnard b (Barnard's Star b),[121] c, d and e,[122] making this system the closest planetary system to host multiple planets Reported for reference.
	CoRoT-1b	1.805 +0.132 −0.131[76]	←	1.03 ± 0.12[76]	First exoplanet for which optical (as opposed to infrared) observations of phases were reported.[123]
	WTS-2b	1.804 +0.144 −0.158[76]	←	1.12 ± 0.16[76]
	WASP-76b	1.802±0.042[113]	←	0.921±0.032[113]	A glory effect in the atmosphere of WASP-76b might be responsible for the observed increase in brightness of its eastern terminator zone which if confirmed, it would become the first exoplanet to have its glory-like phenomenon to be discovered.[124][125] WASP-76b is suspected to have an exomoon analogue to Jupiter's Io due to the detection of sodium via absorption spectroscopy.[126]
	Saffar (υ And Ab)	~1.8[127]	←	1.70 +0.33 −0.24[128]	Radius estimated using the phase curve of reflected light. The planet orbits very close to Titawin (υ And A) at the distance of 0.0595 AU, completing an orbit in 4.617 days.[129] First multiple-planet system to be discovered around a main-sequence star, and first multiple-planet system known in a multiple-star system.
	HAT-P-40b	1.799 +0.237 −0.260[76]	←	0.48 ± 0.13[76]	A very puffy hot Jupiter
	WASP-122b (KELT-14b)	1.795 +0.107 −0.079[76]	←	1.284 ± 0.032[130]
	KELT-12b	1.79 +0.18 −0.17[131]	←	0.95 ± 0.14[131]
	Tylos (WASP-121b)	1.773 +0.041 −0.033[132]	←	1.157 ± 0.07[132]	First exoplanet found to contain water on its stratosphere. Tylos is suspected to have an exomoon analogous to Jupiter's Io due to the detection of sodium absorption spectroscopy around it.[133]
	TOI-640 Ab	1.771 +0.060 −0.056[134]	←	0.88 ± 0.16[134]
	WASP-187b	1.766 ± 0.036[64]	←	0.801 +0.084 −0.083[64]
	WASP-94 Ab	1.761 +0.194 −0.191[76]	←	0.5±0.13[76]
	TOI-2669b	1.76 ± 0.16[135]	←	0.61 ± 0.19[135]
	WISE J0528+0901	1.752 +0.292 −0.195[136]	†	13 +3 −6[136]	Brown dwarf or rogue planet.
	HATS-26b	1.75 ± 0.21[137]	←	0.650 ± 0.076[137]
	Kepler-12b	1.7454 +0.076 −0.072[138]	←	0.431 ± 0.041[139]	Least-irradiated of four Hot Jupiters at the time of discovery
	HAT-P-65b	1.744 +0.165 −0.215[76]	←	0.527 ± 0.083[140]	This planet has been suffering orbital decay due to its close proximity to HAT-P-65; 0.04 AU.[141]
	2MASS J2352-1100	1.742 +0.035 −0.036[105]	†	12.4 +9.4 −5.5[105]	Brown dwarf or rogue planet.
	KELT-15b	1.74 ± 0.20[109]	←	1.31 ± 0.43[109]
	HAT-P-57b	1.74 ± 0.36[109]	←	1.41 ± 1.52[109]
	WASP-93b	1.737 +0.121 −0.170[76]	←	1.47 ± 0.29[76]
	WASP-82b	1.726 +0.163 −0.195[76]	←	1.17 ± 0.20[76]
	Ditsö̀ (WASP-17b)	1.720 +0.004 −0.005, 1.83 ± 0.01[142]	←	0.512 ± 0.037[143]	First planet discovered to have a retrograde orbit[144] and first to have quartz (crystalline silica, SiO2) in its clouds.[145] Has an exteremely low density of 0.08 g/cm3,[144] the lowest of any exoplanet when it was discovered, and was possibly the largest exoplanet at the time of discovery, with a radius of 1.92 RJ.[146]
	KELT-19 Ab	1.717 +0.094 −0.093[113]	←	3.98+0.32 −0.33[113]	First exoplanet found to have its orbit flipped (obliquity of 155 +17 −21°) due to constraints on stellar rotational velocity, sky-projected obliquity and limb-darkening coefficients (see Kozai–Lidov mechanism).[147]
	HAT-P-39b	1.712+0.140 −0.115[76]	←	0.60±0.10[76]
	KELT-4Ab	1.706 +0.085 −0.076[148]	←	0.878 +0.070 −0.067[148]
	Pollera (WASP-79b)	1.704 +0.195 −0.180[76]	←	0.850 +0.180 −0.180[76]
	HAT-P-64b	1.703 ± 0.070[149]	←	0.58 +0.18 −0.13[149]
	WASP-78b	1.70 ± 0.04,[150] 1.93 ± 0.45[54]	←	0.89 ± 0.08[150]	This planet has likely undergone in the past a migration from the initial highly eccentric orbit.[151]
	Qatar-7b	1.70 ± 0.03[54]	←	1.88 ± 0.25[152]
	SSTB213 J041757 b	1.70[153]	†	1.50[153]	In a binary with a larger 2 RJ planet.
	CoRoT-17b	1.694 +0.139 −0.193[76]	←	2.430±0.300[76]
	TOI-615b	1.69+0.06 −0.05[154]	←	0.43+0.09 −0.08[154]
	CoRoT-35b	1.68 ± 0.11[155]	←	1.10 ± 0.37[155]
	TOI-1855 b	1.65 +0.52 −0.37[156]	←	1.133 ± 0.096[156]
	TOI-3807 b	>1.65 (95% lower limit)[157]	→	1.04 +0.15 −0.14[157]	Grazing planet, a large radius of 2.00 RJ derived from transit data is unreliable due to its grazing nature.
	HAT-P-7b (Kepler-2b)	1.64 ± 0.11[158]	←	1.806 ± 0.036[159]	Second planet discovered to have a retrograde orbit (after Ditsö̀)[160][161] and first exoplanet to be detected by ellipsoidal light variations[162]
	NGTS-33 b	1.64 ± 0.07[163]	←	3.6 ± 0.3[163]
	HAT-P-64b	1.631 ± 0.070[149]	←	0.574 ± 0.038[149]
	WASP-82b	1.62 ± 0.13[109]	←	1.17 ± 0.20[109]
	KELT-8b	1.62 ± 0.10[109]	←	0.66 ± 0.12[109]
	WASP-189 b	1.619 ± 0.021[164]	←	1.99 +0.16 −0.14[164]	One of the hottest known exoplanets.
	HAT-P-65b	1.611 ± 0.024[165]	←	0.554 +0.092 −0.091[165]
	K2-52b	1.61 ± 0.20[166]	←	[166]
	NGTS-31 b	1.61 ± 0.16[167]	←	1.12 ± 0.12[167]
	HATS-11b	1.609 ± 0.064[168]	←	0.85[168]
	KELT-7b	1.60 ± 0.06[109]	←	1.39 ± 0.22[109]
	SR 12 c (SR 12 (AB) b, SR 12 C)	~ 1.6,[169] 2.38 +0.27 −0.32[78]	?	11 ± 3[169]	The planet is at the very edge of the deuterium burning limit. This object orbits around SR 12 AB at the distance of 980 AU but has a circumplanetary disk, detected in sub-mm with ALMA.[169] Other sources of masses includes 14 +7 −8 MJ,[170] 12 – 15 MJ[171] and 13 ± 2 MJ.[78]
A few notable examples with radii below 1.6 RJ (17.93 R🜨).
	2M1510 A (2MASSW J1510478 A)	1.575[172] (0.162 R☉)	#	34.676 ± 0.076[173] (0.033101(73) M☉)	Second eclipsing binary brown dwarf system discovered and first kind of system to be directly imaged, orbiting around 20.9 days.[174][172] The members of 2M1510 triple (likely)[173] or quadruple system.[174] Age: 45 ± 5 Myr Have a strong candidate planet, 2M1510 b, that orbits polar around 2M1510AB, making this planet the first planet discovered orbiting polar around a binary system.[173][175][176] Reported for reference.
	2M1510 B (2MASSW J1510478 B)		#	34.792 ± 0.072[173] (0.033212(69) M☉)
	Kepler-7b	1.574 +0.075 −0.071[138]	←	0.433 +0.040 −0.041[177]	One of the first five exoplanets to be confirmed by the Kepler spacecraft, within 34 days of Kepler's science operations,[178] and the first exoplanet to have a crude map of cloud coverage.[179][180][181]
	HD 106906 b	1.54 +0.04 −0.05[182]	←	11 ± 2[183]	This planet orbits around HD 106906 at the distance of 738 AU, a distance much larger than what is possible for a planet formed within a protoplanetary disk.[184] It more likely formed on its own, like a star, rather in a protoplanetary disk.[185] Recent observations made by the Hubble Space Telescope strengthened the case for the planet having an unusual orbit that perturbed it from its host star's debris disk causing NASA and several news outlets to compare to the hypothetical Planet Nine.[186][187]
	2MASS J1115+1937	1.5 ± 0.1[188]	←	6 +8 −4[188]	Nearest rogue planet surrounded by planetary disk at the distance of 147 ± 7 ly (45.1 ± 2.1 pc).[188]
	Proxima Centauri (Alpha Centauri C)	1.50 ± 0.04[189] (0.1542 ± 0.0045 R☉)	#	127.9 ± 2.3[189] (0.1221 ± 0.0022 M☉)	Nearest star and planetary system to the Sun, at a distance of 4.24 ly (1.30 pc), orbiting around Alpha Centauri AB System, the nearest star system to the Sun. Age: 4.85 Gyr.[190] Has a confirmed planet, Proxima Centauri b,[191] a disputed planet, Proxima Centauri c,[192] and a unconfirmed planet, Proxima Centauri d. Reported for reference.
	Beta Pictoris b (β Pic b)	1.46 ± 0.01[193]	←	11.729 +2.337 −2.135[194]	First exoplanet to have its rotation rate measured[195][196] and fastest-spinning planet discovered at the equator speed of 19.9 ± 1.0 km/s (12.37 ± 0.62 mi/s) or 71,640 ± 3,600 km/h (44,520 ± 2,240 mph).[197] Beta Pictoris b is suspected to have exomoon due to the former's predicted obliquity misalignment.[198]
	Najsakopajk (HIP 65426 b)	1.44 ± 0.03[199]	←	7.1 ± 1.2, 9.9 +1.1 −1.8, 10.9 +1.4 −2.0[199]	First exoplanet to be imaged by the James Webb Space Telescope.[200] The JWST direct imaging observations tightly constrained its bolometric luminosity, which provides a robust mass constraint of 7.1 ± 1.2 MJ. The atmospheric fitting of both temperature and radius are in disagreement with evolutionary models. Moreover, this planet is around 14 million years old which is however not associated with a debris disk, despite its young age,[201][202] causing it to not fit current models for planetary formation.[203]
	Banksia (WASP-19b)	1.386 ± 0.032[204]	←	1.168 ± 0.023[204]	First exoplanet to have its secondary eclipse and orbital phases observed from the ground-based observations[205] and first to have titanium oxide (TiO) detected in an exoplanet atmosphere.[206][207]
	HD 209458 b ("Osiris")	1.359 +0.016 −0.019[208]	←	0.682 +0.014 −0.015[208]	Represents multiple milestones in exoplanetary discovery, such as the first exoplanet known observed to transit its host star, the first exoplanet with a precisely measured radius, one of first two exoplanets (other being HD 189733 Ab) to be observed spectroscopically[209][210] and the first to have an atmosphere, containing evaporating hydrogen, and oxygen and carbon. First extrasolar gas giant to have its superstorm measured. Nicknamed "Osiris".
	Teide 1	1.311 +0.120 −0.075[105] (0.1347 +0.0123 −0.0077 R☉)	#	52 +15 −10[105] (0.0496 +0.0143 −0.0095 M☉)	The first brown dwarf to be confirmed.[211][212] It is located in the Pleiades and has an age of 70 – 140Myr.[213] Reported for reference.
	OGLE-TR-56b	1.30 ± 0.05	←	1.29 ± 0.12	First discovered exoplanet using the transit method.[214]
	TOI-157b	1.29 ± 0.02[215]	←	1.18 ± 0.13[215]	Oldest confirmed planet at the age of 12.9 +1.4 −0.69 Gyr[215]
	Bocaprins (WASP-39b)	1.27 ± 0.04[216]	←	0.28 ± 0.03[216]	First exoplanet found to contain carbon dioxide[217][218] and sulfur dioxide[219] in its atmosphere.
	TrES-2 (Kepler-1 Ab)	1.265 +0.054 −0.051[138]	←	1.199 ± 0.052[220]	Darkest known exoplanet due to an extremely low geometric albedo of 0.0136, absorbing 99% of light.
	Dimidium (51 Pegasi b)	1.2 ± 0.1[221]	←	0.46 +0.06 −0.01[222]	First exoplanet to be discovered orbiting a main-sequence star.[223] Prototype of the hot Jupiters.
	HR 8799 b	1.2 ± 0.1[224]	←	5 +2 −1[225]	First directly imaged planetary system having multiple exoplanets. HR 8799 e is also first exoplanet to be directly observed using optical interferometry. All four planets will cool and shrink to about the same size as Jupiter's.
	HR 8799 c		←	7 +3 −2[225]
	HR 8799 d		←	7 +3 −2[225]
	HR 8799 e	1.17 +0.13 −0.11[226]	←	9.6 +1.9 −1.8[227]
	Ahra (WD 0806-661 b)	1.17 ± 0.07[228]	←	6.8 – 9.0[229]	First exoplanet discovered around a single (as opposed to binary) white dwarf, and the coldest directly imaged exoplanet when discovered.[230] Possibly formed closer to Maru (WD 0806−661) when it was a main sequence star, this object migrated further away as it reached the end of its life (see stellar evolution), with a current separation of about 2500 AU. Might be considered an exoplanet or a sub-brown dwarf, the dimmest sub-brown dwarf. The IAU considers objects below the ~13 MJ limiting mass for deuterium fusion that orbit stars (or stellar remnants) to be planets, regardless on how they formed.[231]
	TRAPPIST-1	1.16 ± 0.01[232] (0.1192 ± 0.0013 R☉)	#	94.1 ± 2.4[232] (0.0898 ± 0.0023 M☉)	Coldest and smallest known star hosting exoplanets.[233] All seven exoplanets are rocky planets, orbiting closer to the star than Mercury. Their orbits' inclinations of 0.1 degrees[234] makes TRAPPIST-1 system the flattest planetary system.[235] Age: 7.6 ± 2.2 Gyr.[236] Reported for reference.
	HD 189733 Ab	1.138 ± 0.027[208]	←	1.123 ± 0.045[208]	First exoplanet to have its thermal map constructed,[237] its overall color (deep blue) determined,[238][239] its transit viewed in the X-ray spectrum, one of first two exoplanets (other being "Osiris") to be observed spectroscopically[209][210] and first to have carbon dioxide confirmed as being present in its atmosphere. Such the rich cobalt blue[240][241] colour of HD 189733 Ab may be the result of Rayleigh scattering. The wind can blow up to 8,700 km/h (5,400 mph) from the day side to the night side.[242]
	SWEEPS-11	1.13 ± 0.21[243]	←	9.7 ± 5.6[243]	One of two most distant planets (other being SWEEPS-04) discovered at a distance of 27 710 ly (8500 pc).[244]
	2M1207 b (TWA 27b)	1.13[245]	†	5.5 ± 0.5[245]	First planetary body discovered via direct imaging, and the first around a brown dwarf.[246][247] It could be considered a sub-brown dwarf due to its large mass in relation to its host: 2M1207 b is around six times more massive than Jupiter, but orbits a 26 MJ brown dwarf, a ratio much larger than the 1:1000 of Jupiter and Sun for example. The IAU defined that exoplanets must have a mass ratio to the central object less than 0.04,[248][249] which would make 2M1207b a sub-brown dwarf. Nevertheless, 2M1207b has been considered an exoplanet by press media and websites,[250][251][252] exoplanet databases[253][254] and alternative definitions.[255] It will shrink to a size slightly smaller than Jupiter as it cools over the next few billion years.
	WASP-47 b	1.128 ± 0.013[256]	←	1.144 ± 0.023[257]	Rocky WASP-47 e orbits even closer than hot Jupiter WASP-47 b and both super Earth WASP-47 d and hot Neptune WASP-47 c orbit further than the hot Jupiter, making WASP-47 system the only planetary system to have both planets near the hot Jupiter and another planet much further out.[258]
	2MASS J0523−1403	1.126 ± 0.063[259] (0.116 ± 0.006 R☉)	#	103 ± 11[259] (0.0983 ± 0.0011 M☉) or 67.54 ± 12.79[260] (0.0644 ± 0.0122 M☉)	Coolest main sequence star with effective temperature 1939 K (1666 °C; 3031 °F)[260] and one of the smallest stars, in both radius and mass.[261] Reported for reference.
	Gliese 900 b (CW2335+0142)	1.11[262]	←	10.5[263]	This exoplanet has the largest observed host star separation of any known exoplanet, at 12 000 AU (0.058 pc; 0.19 ly) and the longest known orbital period, at a duration of 1.27 Myr. First confirmed and third discovered circumtriple planet.
	CoRoT-3 Ab	1.08 ± 0.05[264]	*	21.66 ± 1.00[265]	Might be considered either a planet or a brown dwarf, depending on the definition chosen for these terms. If the brown dwarf/planet limit is defined by mass regime using the deuterium burning limit as the delimiter (i.e. 13 MJ), CoRoT-3b is a brown dwarf.[266] If formation is the criterion, CoRoT-3 Ab may be a planet given that some models of planet formation predict that planets with masses up to 25–30 Jupiter masses can form via core accretion.[267] However, it is unclear which method of formation created CoRoT-3A b.
	Kepler-1647 b	1.05932 ± 0.01228[268]	←	1.52 ± 0.65[268]	Longest transit orbital period of any confirmed transiting exoplanet discovered at the duration of 1107 days[269] and largest circumbinary planet discovered.[270] This planet is located within the habitable zone of binary star system Kepler-1647 and thus could theoretically have a habitable Earth-like exomoon.[271]
	Kepler-90h	1.01 ± 0.09[272]	←	0.639 ± 0.016[273]	Located in the Kepler-90 system with eight known exoplanets, whose architecture is similar to that of the Solar System, with rocky planets being closer to the star and gas giants being more distant. This planet is located at 1.01 AU from its star, which is within the habitable zone of Kepler-90 and thus could theoretically have a habitable Earth-like exomoon.
	Jupiter	1 (11.209 R🜨)[k][5] (71 492 km)	#	1 (317.827 M🜨)[274] (1.898 125 × 1027 kg)	Oldest, largest and most massive planet in the Solar System;[275] this planet hosts 95 known moons including the Galilean moons. Reported for reference.
For smaller exoplanets, see the list of smallest exoplanets or other lists of exoplanets. For exoplanets with milestones, see the list of exoplanet extremes and list of exoplanet firsts.

Notes

1. The measured radius from 2003 to 2006 was 696,342 ± 65 kilometers^[6] with some in 2018 measured 695,660 ± 140 kilometers.^[7] To avoid confusion, International Astronomical Union set the solar radius to exactly 695700 km.^[8]
2. The best estimate mass is (1.988475 ± 0.000092) × 10³⁰ kg.^[5] Another estimate mass gave 1.988420 × 10³⁰ kg. (based of the ratio of the mass of Earth to the Sun of 1⁄332946)^[9] To simplify the solar mass, International Astronomical Union set the solar mass to exactly 1.988416 × 10³⁰ kg.^[8]
3. Applying the Stefan–Boltzmann law with a nominal solar effective temperature of 5,772 K:

   ${\displaystyle {\sqrt {{\biggl (}{\frac {5,772}{2,450}}{\biggr )}^{4}\cdot 0.021}}=0.782\ R_{\odot }}$.

4. Using PMS evolutionary models and a potential higher age of 1 Myr, the luminosity would be lower, and the planet would be smaller. However, this would require for the object to be closer as well, which is unlikely. Another distance estimate to the Orion Nebula Cluster would result in a luminosity 1.14 times lower and also a smaller radius.
5. Instead of a photo-evaporating disk it may be an evaporating gaseous globule (EGG). If so, it has a final mass of 2 - 28 M_J.^[15]
6. A calculated radius thus does not need to be the radius of the (dense) core.
7. Proplyd 133-353 is proposed to have formed in a very low-mass dusty cloud or an evaporating gas globule as a second generation of star formation, which can explain both its young age and the presence of its disk.
8. ^{[d] [e] [f] [g] [15]}
9. Based on the estimated temperature and luminosity via the Stefan-Boltzmann law.
10. This radius estimate might have been affected the planet's circumplanetary disk, as the spectrum does not necessarily corresponds to a planet photosphere.
11. Refers to the level of 1 bar atmospheric pressure

Candidates for largest exoplanets

Unconfirmed exoplanets

These planets are also larger than 1.6 times the size of the largest planet in the Solar System, Jupiter, but have yet to be confirmed or are disputed.
Note: Some data may be unreliable or incorrect due to unit or conversion errors

Key (Classification)

←	Probably planets (≲ 13 MJ) (based on mass)
X	Unclassified object (unknown mass)
–	Theoretical planet size restrictions

Key (Illustration)

	Artist's impression
	Direct imaging telescopic observation

Illustration	Name (Alternates) (Status)	Radius (RJ)	Key	Mass (MJ)	Notes
	New born planet limit	~ 30[276]	–	≤ 20 (≤ 13)[276]	Theoretical size limit of a newly-formed planet.
	Young Hot Jupiter limit	~ 20[277]	–	≤ 10[277]	Theoretical size limit of a newly-formed planet that needed 104 – 105 (10000 – 100000) years to migrate close to the host star, but has not yet interacted with it beforehand.
	FU Orionis North b (FU Ori Ab) (unconfirmed)	~ 9.8[276] (~ 1.0 R☉)	←	~ 3[276]	Discovered using a variation of disk kinematics.[278] Tidal disruption and extreme evaporation made the planet radius shrink from the beginning of the burst (14 RJ) in 1937[277] to the present year by ~30 per cent and its mass is around half of its initial mass of 6 MJ.[277][276]
	UCAC4 174-179953 b (unclassified)	8.14 ± 0.40[279] (0.84 R☉)	X	Unknown	Object cannot be classified as brown dwarf or exoplanet without a mass estimate.
	UCAC4 220-040923 b (unclassified)	4.65 ± 0.20[279]	X	Unknown
	UCAC4 223-042828 b (unclassified)	3.33 ± 0.50[279]	X	Unknown
	UCAC4 185-192986 b (unclassified)	3.3 ± 0.2[279]	X	Unknown
	UCAC4 118-126574 b (unclassified)	3.12 ± 0.10[279]	X	Unknown
	UCAC4 171-187216 b (unclassified)	2.75 ± 0.20[279]	X	Unknown
	KOI-7073 b (unclassified)	2.699 +0.473 −0.794[280]	X	Unknown
	UCAC4 175-188215 b (unclassified)	2.69 ± 0.50[279]	X	Unknown
	UCAC4 116-118563 b (unclassified)	2.62 ± 0.10[279]	X	Unknown
	19g-2-01326 b (unclassified)	2.29 +0.13 −0.61[281]	X	Unknown
	SOI-2 b (unclassified)	2.22[282]	X	Unknown
	TIC 332350266.01 (unclassified)	2.21±3.18[283]	X	Unknown
	Old Hot Jupiter limit	2.2[63]	–	> 0	Theoretical limit for hot Jupiters close to a star, that are limited by tidal heating, resulting in 'runaway inflation'
	TIC 138664795.01 (unclassified)	2.16 ± 0.16[283]	X	Unknown	Object cannot be classified as brown dwarf or exoplanet without a mass estimate.
	UCAC4 221-041868 b (unclassified)	2.1 ± 0.20[279]	X	Unknown
	TOI-496 b (unclassified)	2.05 +0.63 −0.29[284]	X	Unknown
	SOI-7 b (unclassified)	1.96[282]	X	Unknown
	UCAC4 121-140615 b (unclassified)	1.94 ± 0.20[279]	X	Unknown
	UCAC4 123-150641 b (unclassified)	1.93 ± 0.20[279]	X	Unknown
	TIC 274508785.01 (unclassified)	1.92±2.37[283]	X	Unknown
	W74 b (Gaia DR2 6045477635223138432 b) (unclassified)	1.9[285]	X	Unknown
	TIC 116307482.01 (unclassified)	1.89 ± 1.46[283]	X	Unknown
	UCAC4 122-142653 b (unclassified)	1.85 ± 0.10[279]	X	Unknown
	TIC 77173027.01 (unclassified)	1.84 ± 1.12[283]	X	Unknown
	TOI-159 Ab (unclassified)	1.80 ± 0.77[286]	X	Unknown
	TIC 82205179.01 (TIC 82205179 b) (unclassified)	1.76 ± 0.56[283]	X	Unknown
	UCAC4 124-144273 b (unclassified)	1.71 ± 0.10[279]	X	Unknown
	TOI-710 b (unclassified)	1.66 ± 1.10[287]	X	Unknown
Exoplanets with known mass of >1 MJ but unknown radius
	BD+20 2457 b (unconfirmed)	Unknown	←	13[288]	The chemical abundances of BD+20 2457 system suggest that the star formed from the Milky Way Galaxy protodisk. Alternatively, it could have formed from debris of the Gaia-Enceladus galaxy as it merged with the Milky Way. If BD+20 2457 formed from the Gaia-Enceladus debris, then the planets could have an extragalactc origin.[288]
	BD+20 2457 c (unconfirmed)	Unknown	←	7[288]
	PA-99-N2 b (unconfirmed)	Unknown	←	6.34[289]	Candidate extragalactic planet; One possibility for the event is that a star in the disk of Andromeda Galaxy gravitationally lensed a red giant also in the disk. In this case the lens profile makes it likely that the star has a planet.[289][290] A similar event was seen in 1996 when a team of astronomers discovered an anomalous fluctuation in the Twin Quasar's lightcurve that seemed to be caused by a planet approximately 3 M🜨 in size in the quasar's lensing galaxy YGKOW G1. However, the results remain speculative because the chance alignment that led to its discovery will never happen again.[291]
	Thestias (Pollux b, β Gem b, HD 62509 b) (disputed)	Unknown	←	2.30 ± 0.45[292]	Suspected orbiting around Pollux in 1993,[293] Thestias was discovered in 2006,[292] (supported by another study in 2008)[294] however, its existence has since been disputed due to its proposed period of Thestias being close to the stellar rotation period.[295][296]

Exoplanets with uncertain radii

This list contains planets with uncertain radii that could be below or above the adopted cut-off of 1.6 R_J, depending on the estimate.

Key (Classification)

←	Probably planets (≲ 13 MJ) (based on mass)
?	Status uncertain (inconsistency in age or mass of planetary system)
→	Planets with grazing transit, hindering radius determination

Key (Illustration)

	Direct imaging telescopic observation

Illustration	Name (Alternates)	Radius (RJ)	Key	Mass (MJ)	Notes
	AB Pictoris b (AB Pic b)	1.57 ± 0.07 – 1.8 ± 0.3[297]	←	10 ± 1[297]	Previously believed to be a likely brown dwarf, with mass estimates of 13–14 MJ[298] to 70 MJ,[299] its mass is now estimated to be 10±1 MJ, with an age of 13.0+1.1 −0.6 million years.[300]
	TOI-2193 Ab	>1.55 (95% lower limit)[301]	→	0.94 ± 0.18[301]	Grazing planet, a large reported radius of 1.77 RJ is unreliable. Whether it is larger than 1.6 RJ is unknown.
	TOI-3540 b	>1.44 (95% lower limit)[301]	→	1.18 ± 0.14[301]	Grazing planet, a large reported radius of 2.10 RJ is unreliable. Whether it is larger than 1.6 RJ is unknown.
	TOI-1408 b	>1, 1.5 (estimate),[302] 2.23 ± 0.36,[a] 2.4 ± 0.5[303]	→	1.86 ± 0.02[303]	A large radius of 2.23–2.4 RJ has been derived from transit photometry,[303] but this value is likely inaccurate due to the grazing transit of TOI-1408 b; it transits only part of the star's surface, thus hindering a precise measurement of planet-to-star size ratio. Only a lower limit of about 1 RJ can be obtained, whether TOI-1408 b is larger than 1.6 RJ is unknown.[302]

Notes

1. Converted from 25±4 R_🜨.

Chronological list of largest exoplanets

These exoplanets were the largest at the time of their discovery.
Present day: 24 April 2025

Key (Classification)

*	Later identified to be a probable/confirmed brown dwarf (≳ 13 MJ) or a star (≳ 82.76 MJ)
†	Candidate for largest exoplanet (currently or in time span)
?	Status uncertain (inconsistency in age or mass of planetary system) while being candidate for largest exoplanet
→	Assumed largest exoplanet, while unconfirmed, later retracted or later confirmed
←	Largest exoplanet (≲ 13 MJ) at the time
–	Largest confirmed exoplanet (in radius and mass), while discovered candidates might be larger
#	Non-exoplanets reported for reference

Key (Illustration)

	Artist's impression
	Artist's impression size comparison
	Direct Imaging telescopic observation
	Transiting telescopic observation
	Graphic chart

Years largest discovered	Illustration	Name (Alternates)	Radius at that time (RJ)	Key	Mass (MJ)	Notes
(2025 – present)		AB Aurigae b (AB Aur b, HD 31293 b)	2.75[42]	*	20[43][47]	The commonly favored model for gas giant planet formation – core accretion – has significant difficulty forming massive gas giant planets at AB Aur b's very large distance from its AB Aur. Instead, AB Aur b may be forming by disk (gravitational) instability,[304] where as a massive disk around a star cools, gravity causes the disk to rapidly break up into one or more planet-mass fragments.[305] A more recent study revised the apparent magnitude, making AB Aur b more likely to be brown dwarf.[47]
2024 – present		XO-6b	2.17 ± 0.2[64]	–	4.47 ± 0.12[64]	A very puffy Hot Jupiter
2024 – 2024		HAT-P-67b	2.165 +0.024 −0.022[a][68]	–	0.418 ± 0.012[64]	A very puffy Hot Jupiter. Previously the largest known planet with an accurately and precisely measured radius,[66] a new estimate revised its radius.[68][64]
(2022 – 2025)		AB Aurigae b (AB Aur b, HD 31293 b)	2.75[42]	?	20 (~ 4 Myr)[43] < 130, 10 – 12 (1 Myr)[42]	The commonly favored model for gas giant planet formation – core accretion – has significant difficulty forming massive gas giant planets at AB Aur b's very large distance from its AB Aur. Instead, AB Aur b may be forming by disk (gravitational) instability,[304] where as a massive disk around a star cools, gravity causes the disk to rapidly break up into one or more planet-mass fragments.[305]
(2020 – present)		PDS 70b	2.7[44]	†	3.2 +3.3 −1.6, 7.9 +4.9 −4.7, < 10 (2 σ), ≲ 15 (total)[84]	Has been later measured to have a radius of only 1.96 RJ,[83] and then 2.7 RJ in 2022.[44] Large size needs confirmation due to this discrepancy.
			1.96[83]
			2.09 +0.23 −0.31 – 2.72 +0.15 −0.17[306]
(2020 – present)		SR 12 c (SR 12 (AB) c, SR 12 C)	2.38 +0.27 −0.32[78]	?	13 ± 2[78]	The planet is at the very edge of the deuterium burning limit. Mass being below it needs confirmation. Other sources of masses includes 14 +7 −8 MJ,[170] 12 – 15 MJ.[171]
2017 – 2024		HAT-P-67b	2.085 +0.096 −0.071[67]	–	0.34 +0.25 −0.19[307]	A very puffy Hot Jupiter. At discovery the largest known planet with an accurately and precisely measured radius.[66]
2017 – 2017		XO-6b	2.07 ± 0.22[308]	–	4.47 ± 0.12[64]	A very puffy Hot Jupiter
(2014 – present)		ROXs 42B b	2.10 ± 0.35[26]	†	9 +6 −3;[71] 10 ± 4[72]	Large size needs confirmation. Other estimates include 1.9 – 2.4 RJ, 1.3 – 4.7 RJ.[73] Other recent sources of masses include 3.2 – 27 MJ,[75] 13 ± 5 MJ.[26]
			2.43 ± 0.18 – 2.55 ± 0.2[74]
2010 – 2017		Ditsö̀ (WASP-17b)	1.74 +0.26 −0.23[144]	–	0.512 ± 0.037[143]	First planet discovered to have a retrograde orbit[144] and first to have quartz (crystalline silica, SiO2) in the clouds of an exoplanet.[145] Puffiest and possibly largest exoplanet at the time of discovery.[146] Extremely low density of 0.08 g/cm3.[144]
(2008 – present)		CT Chamaeleontis b (CT Cha b)	2.20 +0.81 −0.60[52]	*	17 ± 6[52]	Possibly the largest planet.[52]
2007 – 2010		TrES-4 (GSC 02620-00648 Ab)	1.674 ± 0.094[309]	–	0.78 ± 0.19[109][76]	This planet has a density of 0.2 g/cm3, less than Saturn's 0.7 g/cm3.
(2007 – present)		GQ Lupi b (GQ Lup Ab, GQ Lup B)	3.50 +1.50 −1.03[27]	*	1 – 46[310]	First confirmed exoplanet candidate to be directly imaged.
(2006 – present)		DH Tauri b (DH Tau b)	2.7 ± 0.8[28]	†	11.5 +10.5 −3.1[311]	Mass being below the deuterium burning limit needs confirmation. Temperature originally given as 2700 – 2800 K.[312] Other sources give the radii: 2.49 RJ,[34][b] 2.68 RJ,[313] and 2.6 ± 0.6 RJ[26] and masses: 11 ± 3 MJ,[28] 14.2 +2.4 −3.5 MJ,[50] 17 ± 6 MJ[51] and 12 ± 4 MJ[26]
			1.75[311][312][b]
2005 – 2007		HD 209458 b ("Osiris")	1.27 ± 0.02[314]	–	0.682 +0.014 −0.015[208]	First known transiting exoplanet, first precisely measured planet available, first to have its orbital speed measured, determining its mass directly,[315] one of first two exoplanets (other being HD 189733 Ab) to be observed spectroscopically[209][210] and first to have an atmosphere, containing evaporating hydrogen, and first to have contained oxygen and carbon. First extrasolar gas giant to have its superstorm measured. Nicknamed "Osiris".
(2005 – 2007)		GQ Lupi b (GQ Lup Ab, GQ Lup B)	~ 2[316]	†	1 – 46[310]	First confirmed exoplanet candidate to be directly imaged.
1999 – 2005		HD 209458 b ("Osiris")	1.27 ± 0.02[314]	←	0.682 +0.014 −0.015[208]	First known transiting exoplanet, first precisely measured radius available, first to have its orbital speed measured, determining its mass directly,[315] and first to have an atmosphere, containing evaporating hydrogen, and first to have contained oxygen and carbon. First extrasolar gas giant to have its superstorm measured. Nicknamed "Osiris".
(1995 – 1999)		various	Unknown	†	0.49 – 8.35	About 20 – 25 planets including Saffar were found within this time span via the radial velocity method, none of them having radius measurements, especially shortly after their discoveries. As expected, Dimidium is larger than Poltergeist, whether one of the additional planets found till 1999 is larger than Dimidium is not clear to this day.
1995 – 1999		Dimidium (51 Peg b)	Unknown	–	0.46 +0.06 −0.01[222]	First convincing exoplanet discovered orbiting a main-sequence star. Prototype hot Jupiter.
1995 – 1995		Dimidium (51 Peg b)	Unknown	←	0.46 +0.06 −0.01[222]	First convincing exoplanet discovered orbiting a main-sequence star. Prototype hot Jupiter.
(1993 – 1995)		PSR B1620−26 b ("Methuselah")	Unknown	→	2.5 ± 1[317]	Likely larger than Poltergeist, but not confirmed as planet until 2003. First circumbinary planet, first planet to be found in a globular cluster and the oldest planet to be discovered (until 2020) at the age of 11.2–12.7 billion years old,[318] hence the nickname, "Methuselah".[317][319]
1992 – 1995		Poltergeist (PSR B1257+12 c)	Unknown	←	0.013 53 ± 0.000 63 (4.3 ± 0.2 M🜨)[320]	First confirmed planet ever discovered outside the Solar System together with the less massive Draugr (PSR B1257+12 b), one of three pulsar planets known to be orbiting the pulsar Lich (PSR B1257+12).[321][322] Lich planets are likely to form in a second round of planet formation as a result of merger of two white dwarfs into a pulsar star and a resulting disk of material in orbit around the star.[323]
(1991 – 1992)		PSR 1829−10 b (PSR B1829−10 b)	Unknown	→	Unknown	First found "orbiting the neutron star PSR 1829-10"[324] but in 1992 retracted before the discovery of Lich planets due to errors in calculations.[325]
(1989 – 1995)		HD 114762 Ab ("Latham's Planet")	Unknown	*	11.069 ± 0.063,[326] ~63.2[327]	Discovered in 1989 by Latham to have a minimum mass of 11.069 ± 0.063 MJ (at 90°) and a probable mass of approximately 63.2 MJ (at 10°),[327] making the former planet the first to be spotted,[328] and confirmed in 1991, it was thought to be the first discovered exoplanet until 2019 when it was confirmed to be a low-mass star with the mass of 107 +20 −27 MJ[329] (and later reviewed up to 147.0 +39.3 −42.0 MJ in 2020[330] and 306.93 MJ (0.293 M☉) in 2022),[331] making Lich planet the first confirmed exoplanet discovered ever.
(1988 – 1992)		Tadmor (Gamma Cephei Ab, γ Cep Ab)	Unknown	→	6.6 +2.3 −2.8[332]	First evidence for exoplanet to receive later confirmation. First reported in 1988,[333] making it arguably the first true exoplanet discovered, and independently in 1989,[334] however, retracted in 1992[335] due to the possibility that the stellar activity of the star mimics a planet not allowing a solid discovery claim and then finally confirmed in 2003.[336]
(Antiquity – 1992, 1988 or 1995)		Jupiter	1 (11.209 R🜨)[c][5] (71 492 km)	#	1 (317.827 M🜨)[274] (1.898 125 × 1027 kg)	Oldest, largest and most massive planet in the Solar System[275] Observations date back to 7th or 8th century BC. Using an early telescope the Galilean moons were discovered in 1610, the planet hosts 95 known moons. Photograph took in 1879, making Jupiter the first planet to have recognisable photo of a planet. Reported for reference.
For earlier entries, see early speculations and discredited claims.

Notes

1. Calculated using R_p/R_⋆ multiplied by R_⋆. The value is later multiplied by (142984 km ÷ 1391400 km) to convert from R_☉ to R_J.
2. Based on the estimated temperature and luminosity via the Stefan-Boltzmann law.
3. Refers to the level of 1 bar atmospheric pressure

See also

• Lists of planets
• List of smallest exoplanets
• List of largest cosmic structures
• List of largest galaxies
• List of largest nebulae
• List of largest known stars
• Lists of astronomical objects
• List of most massive stars