View source for List of largest exoplanets

{{short description|none}}
[[File:790106-0203 Voyager 58M to 31M reduced.gif|thumb|251x251px|[[Jupiter]] as seen by ''[[Voyager 1]]'' in 1979.  It is the largest [[planet]] having its surface resolved<ref name="8hZ77" /><ref name="EKWXb" /><ref name="UxcVg" /> and it is the largest [[planet]] in the [[Solar System]].<ref name="Ujyhy" />]]
Below is a '''list of the largest [[exoplanet]]s''' so far discovered, in terms of physical size, ordered by radius. 

== 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. Then there is the fact that these objects might be [[brown dwarf]]s, [[sub-brown dwarf]]s, or not exist at all. Because of this, this list only cites the most certain measurements to date and is prone to change.

== List==
The sizes are listed in units of [[Jupiter radius|Jupiter radii]] ({{Jupiter radius}}, 71 492&nbsp;''km''). This list is designed to include all planets that are larger than 1.6 times the size of [[Jupiter]]. Some well-known planets that are smaller than {{Jupiter radius|1.6}} ({{#expr: (71492 * 1.6) / 6378 round 2}}{{Nbsp}}{{Earth radius|link=y}} or {{val|{{#expr: 71492 * 1.6 round 3}}}} ''{{val|u=km}}'') have been included for the sake of comparison. 
<div style="display:inline-grid; >
{| class="wikitable" style="margin:0px 15px 0px 0px"
|+Key (classification)
|-
| bgcolor="#FFF8DC" width=50px style="text-align:center;"|{{asterisk}}
! Probably brown dwarfs (≳ 13 {{Jupiter mass}}) (based on mass)
|-
| bgcolor="#FFE8DC" width=50px style="text-align:center;"|{{dagger}}
! Probably sub-brown dwarfs (based on mass and location)
|-
| bgcolor="#CFF7C1" width=50px style="text-align:center;"|?
! Uncertain status (inconsistency in age or mass of planetary system)
|-
| bgcolor="#D1E231" width=50px style="text-align:center;"|!
! Uncertain status while probably brown dwarfs (≳ 13 {{Jupiter mass}}) (based on mass)
|-
| style="text-align:center;"| ←
! Probably exoplanets (≲ 13 {{Jupiter mass}}) (based on mass)
|-
| bgcolor="#CEE0F2" width="50px" style="text-align:center;" | →
! Planets with grazing transit, hindering radius determination
|-
| bgcolor="pink" width=50px style="text-align:center;" |{{number sign}}
! Notable non-exoplanets reported for reference
|-
| bgcolor="#e6e6e6" width=50px style="text-align:center;"| –
! Theoretical planet size restrictions
|}
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<div style=display:inline-grid>
{| class="wikitable"
|+Key (illustration)
|-
| style="border:4px ridge red;"|
! Artist's impression
|-
| style="border:4px ridge yellow;"|
! Artist's size comparison
|-
| style="border:4px ridge orange;"|
! Artist's impression size comparison
|-
| style="border:4px ridge blue;"|
! Direct imaging telescopic observation
|-
| style="border:4px ridge cyan;"|
! Direct image size comparison
|-
| style="border:4px ridge green;"|
! Composite image of direct observations
|-
| style="border:4px ridge purple;"|
! Transiting telescopic observation
|-
| style="border:4px ridge pink;"|
! Simulation observation
|}
</div>
{{sticky header}}
{| class="wikitable sortable sticky-header"
|-
! class="unsortable"| Illustration
! Name<br />''(Alternates)''
! data-sort-type=number| Radius <br />({{Jupiter radius|link=y}})
! class="unsortable"| Key
! data-sort-type=number| Mass <br />({{Jupiter mass|link=y}})
! class="unsortable" | Notes
|- style="background:pink;"
|style="border:4px ridge blue; background:#000000; text-align:center;"|[[File:The Sun in white light.jpg|112x112px]]
| [[Sun]]<br />''(Sol)''
| data-sort-value="9.731"|{{val|9.731}}<br />({{val|1|ul=Solar radius}})<ref name="Prša-2016">{{Cite journal |last1=Prša |first1=Andrej |last2=Harmanec |first2=Petr |last3=Torres |first3=Guillermo |last4=Mamajek |first4=Eric |last5=Asplund |first5=Martin |last6=Capitaine |first6=Nicole |last7=Christensen-Dalsgaard |first7=Jørgen |last8=Depagne |first8=Éric |last9=Haberreiter |first9=Margit |last10=Hekker |first10=Saskia |last11=Hilton |first11=James |last12=Kopp |first12=Greg |last13=Kostov |first13=Veselin |last14=Kurtz |first14=Donald W. |last15=Laskar |first15=Jacques |date=2016-08-01 |title=NOMINAL VALUES FOR SELECTED SOLAR AND PLANETARY QUANTITIES: IAU 2015 RESOLUTION B3 * † |journal=The Astronomical Journal |volume=152 |issue=2 |page=41 |arxiv=1605.09788 |bibcode=2016AJ....152...41P |doi=10.3847/0004-6256/152/2/41 |doi-access=free |issn=0004-6256}}</ref><br />[[Solar radius|''(695 700 km)'']]
| style="text-align:center;" |{{number sign}}
| data-sort-value="1047.569"|1047.569<br />({{val|1|ul=Solar mass}})<ref name="Prša-2016" /><br />''[[Solar mass|(1.988 416 x 10<sup>30</sup> kg)]]''
| The only star in the [[Solar System]]. Responsible for [[life]] on [[Earth]] and keeping the [[Solar System planets|planet]]s on orbit. Age: 4.6 [[Gigayear|Gyr]].<ref name="Bonanno">{{Cite journal |last1=Bonanno |first1=A. |last2=Schlattl |first2=H. |last3=Paternò |first3=L. |year=2002 |title=The age of the Sun and the relativistic corrections in the EOS |journal=[[Astronomy and Astrophysics]] |volume=390 |issue=3 |pages=1115–1118 |arxiv=astro-ph/0204331 |bibcode=2002A&A...390.1115B |doi=10.1051/0004-6361:20020749 |s2cid=119436299}}</ref><br /><small>''Reported for reference.''</small>
|- style="background:pink;"
|style="border:4px ridge red; background:#000000; text-align:center;"|[[File:Artist’s_impression_of_a_planet_around_Alpha_Centauri_B_(symbolic,_annotated).jpg|112x112px]]
| [[Toliman]]<br />''(Alpha Centauri B)''
| data-sort-value="8.3599021"|{{val|8.360}} ± 0.035<ref name="Akeson2021" /><br />(0.8591 ± 0.0036 {{Solar radius|link=y}})
| style="text-align:center;" |{{number sign}}
| data-sort-value="952.4497348"|952.450 ± 2.619<ref name="Akeson2021" /><br />(0.9092 ± 0.0025 {{Solar mass|link=y}})
| One of first two stars (other being [[Rigil Kentaurus|Rigil Kentaurus / Alpha Centauri A]]) to have its [[stellar parallax]] measured.<ref name=Henderson1839>{{Cite journal|last=Henderson|first=Thomas|date=1839|title=On the Parallax of α Centauri|journal=Monthly Notices of the Royal Astronomical Society|volume=4|issue=19 |pages=168–170|doi=10.1093/mnras/4.19.168 |bibcode=1839MNRAS...4..168H|doi-access=free}}</ref> Nearest [[binary star system]] and [[List of nearest stars|nearest stellar system]] to the Sun at the distance of {{cvt|4.344 ± 0.002|ly|pc|lk=on|abbr=off}}. A member of [[Alpha Centauri System]], the nearest system to the Sun. Age: 5.3 ± 0.3 [[Gigayear|Gyr]].<ref name=joyce>{{cite journal |last1=Joyce |first1=M. |last2=Chaboyer |first2=B. |year=2018 |title=Classically and asteroseismically constrained 1D stellar evolution models of {{nobr|α Centauri A}} and B using empirical mixing length calibrations |journal=[[The Astrophysical Journal]] |volume=864 |issue=1 |page=99 |arxiv=1806.07567 |bibcode=2018ApJ...864...99J |doi=10.3847/1538-4357/aad464 |doi-access=free |s2cid=119482849}}</ref><br /><small>''Reported for reference.''</small>
|-style="background:#e6e6e6"
|style="border:4px ridge red; background:black; text-align:center;" |[[File:NASA-ExocometsAroundBetaPictoris-ArtistView.jpg|112x112px]]
| ''Maximum size of [[planetary-mass object]]''
| data-sort-value="8"|8<ref name="Chabrier-2014" />
| style="text-align:center;"|–
| data-sort-value="5"|~ 5<ref name="Chabrier-2014" />
| Maximum theoretical size limit assumed for a ~ 5 {{val|ul=Jupiter mass}} mass object right after formation, however, for 'arbitrary initial conditions'.
|- style="background:#FFE8DC"
|style="border:4px ridge green; background: #000000; text-align:center;"|[[File:Proplyd 133-353 HST F775W image.jpg|112px]]
| [[Proplyd 133-353]]
| data-sort-value="7.82"|≲ 7.82 ± 0.81<ref name="Fang-2016" />{{efn|Applying the [[Stefan–Boltzmann law]] with a nominal [[sun|solar]] [[effective temperature]] of 5,772&nbsp;[[Kelvin|K]]: 
:<math>\sqrt{\biggl(\frac{5,772}{2,450}\biggr)^4 \cdot 0.021} = 0.782\ R_\odot</math>.}}<br />(≲ {{Solar radius calculator|0.021|2450|type=LT|decimals=3|Terr=50|Lerr=0.004|unit=Y|link=Y}})
| style="text-align:center;" |{{dagger}}
| data-sort-value="13.001"|(≲) 13<ref name="Fang-2016" />
| A candidate [[sub-brown dwarf]] or [[rogue planet]] with a [[Photoevaporation|photoevaporating]] disk, located in the [[Orion Nebula|Orion Nebula Cluster]]. At a probable age younger than 500 000 years, it is one of the [[List of exoplanet extremes#Planetary characteristics|youngest]] free-floating [[planetary-mass object|planetary-mass candidates]] known.<ref name="Fang-2016" /><br />More information about Proplyd 133-353 and estimates of its radius are available:{{efn|
{{Efn|1=Using PMS evolutionary models and a potential higher age of 1 [[Megayear|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.}}
{{Efn|Instead of a photo-evaporating disk it may be an evaporating gaseous globule (EGG). If so, it has a final mass of 2 - 28 {{Jupiter mass}}.<ref name="Fang-2016" />|name=Info 2}}
{{Efn|A calculated radius thus does not need to be the radius of the (dense) core. |name=Info 3}}
{{Efn|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.}}
<ref name="Fang-2016" />}}
|- style="background:pink;"
|style="border:4px ridge red; background:#5E2113; text-align:center;" rowspan="2" |[[File:2MASS J05352184–0546085.tif|112x112px]]
| [[2M0535-05|2M0535-05 A]]<br>''(V2384 Orionis A)''
| data-sort-value="6.71"|6.71 ± 0.11<ref name="Gómez Maqueo Chew-2009" /><br />{{nowrap|(0.690 ± 0.011 {{val|ul=Solar radius}})}}
| style="text-align:center;" |{{number sign}}
| data-sort-value="59.9"|59.9 ± 3.5<ref name="Gómez Maqueo Chew-2009" /><br />(0.0572 ± 0.0033 {{val|ul=Solar mass}})
| rowspan="2" |First [[eclipsing binary]] [[brown dwarf]] system to be discovered, orbiting around 9.8 days.<ref name=Stassun2006>{{cite journal |last1=Stassun |first1=Keivan G. |last2=Mathieu |first2=Robert D. |last3=Valenti |first3=Jeff A. |date=March 2006 |title=Discovery of two young brown dwarfs in an eclipsing binary system |journal=[[Nature (journal)|Nature]] |volume=440 |issue=7082 |pages=311–314 |doi=10.1038/nature04570 |pmid=16541067 |bibcode=2006Natur.440..311S}}</ref><ref name=hubblesite2006>{{cite web |url=https://hubblesite.org/contents/news-releases/2006/news-2006-11.html |title=Astronomers Measure Precise Mass of a Binary Brown Dwarf |date=15 March 2006 |website=hubblesite.org |publisher=[[STScI]] |access-date=8 May 2024}}</ref> Age: ~1 [[Million years ago|Myr]]<ref name=":21">{{Cite journal |last1=Gómez Maqueo Chew |first1=Yilen |last2=Stassun |first2=Keivan G. |last3=Prša |first3=Andrej |last4=Mathieu |first4=Robert D. |date=2009-07-10 |title=Near-Infrared Light Curves of the Brown Dwarf Eclipsing Binary 2Mass J05352184-0546085: Can Spots Explain the Temperature Reversal? |url=https://iopscience.iop.org/article/10.1088/0004-637X/699/2/1196 |journal=The Astrophysical Journal |volume=699 |issue=2 |pages=1196–1208 |arxiv=0905.0491 |bibcode=2009ApJ...699.1196G |doi=10.1088/0004-637X/699/2/1196 |issn=0004-637X}}</ref><br /><small>''Reported for reference.''</small>
|- style="background:pink;"
| [[2M0535-05|2M0535-05 B]]<br>''(V2384 Orionis B)''
| data-sort-value="5.25" |5.25 ± 0.09<ref name="Gómez Maqueo Chew-2009" /><br />(0.540 ± 0.009 {{val|ul=Solar radius}})
| style="text-align:center;" |{{number sign}}
| data-sort-value="38.3" |38.3 ± 2.3<ref name="Gómez Maqueo Chew-2009" /> <br />(0.0366 ± 0.0022 {{val|ul=Solar mass}})
|- style="background:#FFE8DC"
|
| [[KPNO-Tau-4]] 
| data-sort-value="4.1"|4.1<ref name="Kraus-2006" /><ref name="l60e2" />
| style="text-align:center;" |{{dagger}}
| data-sort-value="10.502"|10.5<ref name="Kraus-2006" />
| A member of Taurus-Auriga star-forming region.<ref name="l60e2" />
|- style="background:#FFF8DC"
| style="border:4px ridge blue; background:#000000; text-align:center;" |[[File:The Sub-Stellar Companion to GQ Lupi.jpg|112x112px]]
| [[GQ Lupi b]] <br />''(GQ Lupi Ab,<br />GQ Lupi B)''
| data-sort-value="3.0" |3.77<ref name="WDjss" />
| style="text-align:center;" |{{asterisk}}
| data-sort-value="20.001" |20 ± 10;<ref name="Sun-2024" /> <br />{{nowrap|1 – 46}}<ref name="Neuhauser2008" />
| First confirmed [[exoplanet]] candidate to be directly imaged. <!-- 2M1207 b was confirmed few months later --> GQ Lupi b has a mass of 1 – {{Val|46|ul=Jupiter mass}}; 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.<ref name="Alcala2020">{{cite journal |last=Alcalá |first=J. M. |display-authors=etal |year=2020 |title=2MASS J15491331-3539118: a new low-mass wide companion of the GQ Lup system |url=https://www.researchgate.net/publication/339147825 |journal=Astronomy & Astrophysics |volume=635 |pages=L1 |arxiv=2001.10879 |bibcode=2020A&A...635L...1A |doi=10.1051/0004-6361/201937309 |s2cid=210942917}}</ref> Other sources of the radius include {{val|3.7|0.7}} {{Jupiter radius|link=y}},<ref name="Xuan-2024" /> {{val|3.0|0.5}} {{Jupiter radius|link=y}},<ref name="Neuhauser2008" /> {{val|3.5|1.50|1.03}} {{Jupiter radius|link=y}},<ref name="Seifahrt07" /> 4.6 ± 1.4 [[Jupiter radius|''R''<sub>J</sub>]], 6.5 ± 2.0 [[Jupiter radius|''R''<sub>J</sub>]].<ref name="zhou2014" /> 
|- style="background:#FFF8DC"
| style="border:4px ridge blue; background:#000000; text-align:center;"|[[File:View of the dust disc around the young star HD 100546.jpg|112x112px]]
| [[HD 100546 b]]<br />''(KR Muscae b)''
| data-sort-value="3.4"|3.4<ref name="elena" />
| style="text-align:center;" |{{asterisk}}
| data-sort-value="25"|25<ref name="elena" />
| Sometimes the initially reported {{val|6.9}} {{±|2.7|2.9}} {{Jupiter radius|link=y}} for the emitting area due to the diffuse dust and gas envelope or [[debris disk]] surrounding the planet<ref name="quanz2014" /> is confused with the actual radius. Other source of mass: 1.65 {{val|ul=Jupiter mass}}.<ref name="pineda">{{cite journal |last1=Pineda |first1=Jaime E. |last2=Szulágyi |first2=Judit |last3=Quanz |first3=Sascha P. |last4=Van Dishoeck |first4=Ewine F. |last5=Garufi |first5=Antonio |last6=Meru |first6=Farzana |last7=Mulders |first7=Gijs D. |last8=Testi |first8=Leonardo |last9=Meyer |first9=Michael R. |last10=Reggiani |first10=Maddalena |date=2019 |title=High-resolution ALMA Observations of HD 100546: Asymmetric Circumstellar Ring and Circumplanetary Disk Upper Limits |journal=The Astrophysical Journal |volume=871 |issue=1 |page=48 |arxiv=1811.10365 |bibcode=2019ApJ...871...48P |doi=10.3847/1538-4357/aaf389 |doi-access=free}}</ref><br />[[HD 100546]] ''(KR Mus)'' is the nearest [[Herbig Ae/Be star|Herbig Be star]] to the [[Sun]].<ref name="Grady2001">{{Cite journal | title=The Disk and Environment of the Herbig Be Star HD 100546 | last1=Grady | first1=C. A.| last2=Polomski | first2=E. F. | last3=Henning | first3=Th. | last4=Stecklum | first4=B. | last5=Woodgate | first5=B. E. | last6=Telesco | first6=C. M. | last7=Piña | first7=R. K. | last8=Gull | first8=T. R. | last9=Boggess | first9=A. | last10=Bowers | first10=C. W. | last11=Bruhweiler | first11=F. C. | last12=Clampin | first12=M. | last13=Danks | first13=A. C. | last14=Green | first14=R. F. | last15=Heap | first15=S. R. | last16=Hutchings | first16=J. B. | last17=Jenkins | first17=E. B. | last18=Joseph | first18=C. | last19=Kaiser | first19=M. E. | last20=Kimble | first20=R. A. | last21=Kraemer | first21=S. | last22=Lindler | first22=D. | last23=Linsky | first23=J. L. | last24=Maran | first24=S. P. | last25=Moos | first25=H. W. | last26=Plait | first26=P. | last27=Roesler | first27=F. | last28=Timothy | first28=J. G. | last29=Weistrop | first29=D. | display-authors=1 | journal=The Astronomical Journal | volume=122 | issue=6 | pages=3396–3406 | bibcode=2001AJ....122.3396G | doi=10.1086/324447 | year=2001 | doi-access=free}}</ref>
|- style="background:#FFE8DC"
|
| [[2MASS J0437+2331]] 
| data-sort-value="3.30"|3.30<ref name=":17">{{Cite journal |last1=Best |first1=William M. J. |last2=Liu |first2=Michael C. |last3=Magnier |first3=Eugene A. |last4=Bowler |first4=Brendan P. |last5=Aller |first5=Kimberly M. |last6=Zhang |first6=Zhoujian |last7=Kotson |first7=Michael C. |last8=Burgett |first8=W. S. |last9=Chambers |first9=K. C. |last10=Draper |first10=P. W. |last11=Flewelling |first11=H. |last12=Hodapp |first12=K. W. |last13=Kaiser |first13=N. |last14=Metcalfe |first14=N. |last15=Wainscoat |first15=R. J. |date=2017-03-01 |title=A Search for L/T Transition Dwarfs with Pan-STARRS1 and WISE. III. Young L Dwarf Discoveries and Proper Motion Catalogs in Taurus and Scorpius–Centaurus |journal=The Astrophysical Journal |volume=837 |issue=1 |pages=95 |arxiv=1702.00789 |bibcode=2017ApJ...837...95B |doi=10.3847/1538-4357/aa5df0 |doi-access=free |issn=0004-637X}}</ref>{{efn|name=L/Teff|Based on the estimated temperature and luminosity via the [[Stefan-Boltzmann law]].}}
| style="text-align:center;" |{{dagger}}
| data-sort-value="7.1"|7.1 {{±|1.1|1.0}}<ref name=":17" /> 
| May be a [[sub-brown dwarf]] or a [[rogue planet]]
|- style="background:#FFE8DC"
| style="border:4px ridge red; background:#000000; text-align:center;" |[[File:Brown dwarf OTS 44 with disc.jpg|112x112px]]
| [[OTS 44]]
| data-sort-value="3.2"|3.2{{snd}}3.6<ref name="Bonnefoy-2014" />
| style="text-align:center;" |{{dagger}}
| data-sort-value="11.51"|11.5<ref name="LVyQ3" />
| [[Rogue planet#List|First discovered]] [[rogue planet]]; very likely a [[brown dwarf]]<ref name="apj620_1_L51" /> or [[sub-brown dwarf]].<ref name="joergens2013_AA558" /> 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.<ref name="Bonnefoy-2014" />
|- style="background:#FFE8DC"
| style="border:4px ridge blue; background:#000000; text-align:center;" |[[File:Brown dwarf 2M J044144 and planet.jpg|112x112px]]
| [[2MASS J044144b]] <br />''(2M 0441+23 Bb)''
| data-sort-value="3.06"|3.06<ref name="Bowler-2015" />{{efn|name=L/Teff|Based on the estimated temperature and luminosity via the [[Stefan-Boltzmann law]].}}
| style="text-align:center;" |{{dagger}}
| data-sort-value="9.8"|9.8 ± 1.8<ref name="Bowler-2015" />
| Based on the mass ratio to [[2MASS J0441+2301|2M J044145 A]] ''(2M 0441+23 Aa)'' it is likely not a [[exoplanet|planet]] according to the IAU's exoplanet working definition.<ref name="1YDdZ" /> Part of the lowest mass quadruple [[2MASS J0441+2301|2M 0441+23]] system of {{Solar mass|0.26|link=y}}.<ref name="Bowler-2015" />
|- style="background:pink;"
| style="border:4px ridge orange; background:#000000; text-align:center;"|[[File:Kapteyn's Star Comparison.jpg|112x112px]]
| [[Kapteyn's Star]] 
| data-sort-value="2.83"|2.83 ± 0.24<ref name="Guinan-2016" /><br />(0.291 ± 0.025 {{Solar radius|link=y}})
| style="text-align:center;" |{{number sign}}
| data-sort-value="294.4"|294.4 ± 14.7<ref name="Guinan-2016" /><br />(0.2810 ± 0.014 {{Solar mass|link=y}})
| The closest [[Galactic halo|halo]] star and nearest [[red dwarf|red]] [[subdwarf]], at the distance of {{cvt|3.93|pc|ly|2|order=flip}}, 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}} [[Gigayear|Gyr]].<ref name="Kapteyn" /><br /><small>''Reported for reference.''</small>
|- style="background:#D1E231"
| style="border:4px ridge blue; background: white; text-align:center;" |[[File:Subaru AB Aur b.png|112x112px]]
| [[AB Aurigae b]]<br />''(AB Aur b)''
| data-sort-value="2.75" |< 2.75<ref name="Currie-2022" />{{efn|1=This radius estimate might have been affected the planet's circumplanetary disk, as the spectrum does not necessarily corresponds to a planet photosphere.}}
| style="text-align:center;" |!
| data-sort-value="20.001" |20 {{nowrap|(~ 4 [[Megayear|Myr]])}},<ref name="Ginski2022">{{Cite journal |last=Ginski |first=Christian |date=2022-05-09 |title=A massive gas giant caught in formation |url=https://www.nature.com/articles/s41550-022-01665-4 |journal=Nature Astronomy |language=en |volume=6 |issue=6 |pages=639–640 |bibcode=2022NatAs...6..639G |doi=10.1038/s41550-022-01665-4 |issn=2397-3366 |hdl-access=free |hdl=1887/3561614}}</ref><br />{{nowrap|10 – 12}} {{nowrap|(1 [[Megayear|Myr]])}},<br />< 130<ref name="Currie-2022" />
| Likely a [[brown dwarf]]; Assuming a hot-start evolution model and a planetary mass, AB Aurigae b would be younger than 2 [[Megayear|Myr]] to have its observed large luminosity, which is inconsistent with the age of [[AB Aurigae]] of 6.0 {{±|2.5|1.0}} [[Megayear|Myr]], which could be caused by delayed [[planet formation]] in the [[Protoplanetary disk|disk]].<ref name="Zhou2022" /> Other system ages include 1 - 5 [[Megayear|Myr]],<ref name="Currie-2022" /> 4 ± 1 [[Megayear|Myr]]<ref name="d9kt8" /> and 4 [[Megayear|Myr]].<ref name="Herczeg2014">{{Cite journal |last1=Herczeg |first1=Gregory J. |last2=Hillenbrand |first2=Lynne A. |date=2014-04-22 |title=An Optical Spectroscopic Study of T Tauri Stars. I. Photospheric Properties |url=https://iopscience.iop.org/article/10.1088/0004-637X/786/2/97 |journal=The Astrophysical Journal |volume=786 |issue=2 |pages=97 |arxiv=1403.1675 |bibcode=2014ApJ...786...97H |doi=10.1088/0004-637X/786/2/97 |issn=0004-637X}}</ref> Another source gives a higher mass of {{val|20|ul=Jupiter mass}} in the [[brown dwarf]] regime for an age of 4 [[Megayear|Myr]], arguing since gravitational instability of the disk (preferred formation mechanism in the discovery publication)<ref name="Currie-2022" /> operates on very short time scales, the object might be as old as AB Aur.<ref name=Ginski2022 /> A more recent study also support the latter source, given the [[apparent magnitude]] was revised upwards.<ref name=Shibaike2024 />
|-
| style="border:4px ridge blue; background:#000000; text-align:center;"|[[File:DH Tauri.jpg|112x112px]]
| [[DH Tauri b]]<br />''(DH Tau b)''
| data-sort-value="2.701"|2.7 ± 0.8<ref name="zhou2014" />
| style="text-align:center;" |←
| data-sort-value="11.001"|11 ± 3<ref name="zhou2014" />
| First planet to have a confirmed [[circumplanetary disk]], detected with [[polarimetry]] at the [[Very Large Telescope|VLT]]<ref name=":8" /> and [[List of exoplanet extremes#Planetary characteristics|youngest]] confirmed planet at an age of 0.7 [[Myr]].<ref name="Xuan-2024" /> DH Tauri b is suspected to have an [[List of exomoon candidates|exomoon candidate]] orbiting it every 320 years, with about the same mass as Jupiter.<ref name=":7" /><br />Other sources give the radii: {{val|2.6|0.6}} {{Jupiter radius|link=y}},<ref name="Xuan-2024" /> 2.49 {{Jupiter radius|link=y}}<ref name="Bonnefoy-2014" />{{efn|name=L/Teff|Based on the estimated temperature and luminosity via the [[Stefan-Boltzmann law]].}} and masses: 14.2 {{±|2.4|3.5}} {{val|ul=Jupiter mass}},<ref name=":5" /> 17 ± 6 {{val|ul=Jupiter mass}},<ref name=":6" /> 12 ± 4 {{val|ul=Jupiter mass}}.<ref name="Xuan-2024" />
|- style="background:#FFF8DC"
| style="border:4px ridge blue; background:#000000" |[[File:CT Cha B MIRI.jpg|112x112px]]
| [[CT Chamaeleontis b]] <br />''(CT Cha b)''
| data-sort-value="2.6" |2.6 {{±|1.2|0.2}}<ref name="Bonnefoy-2014" />
| style="text-align:center;" |{{asterisk}}
| data-sort-value="17" |17 ± 6<ref name="Schmidt-2008" />
| Likely a brown dwarf.
|- style="background:pink;"
| style="border:4px ridge purple; background:white; text-align:center |[[File:CMDraLightCurve.png|112x112px]]
| [[CM Draconis|CM Draconis A]]<br />''(Gliese 630.1 Aa)'' 
| data-sort-value="2.4437"|2.4437 ± 0.0002<ref name="Martin2024">{{cite journal |last1=Martin |first1=David V. |last2=Sethi |first2=Ritika |display-authors=etal |date=February 2024 |title=The benchmark M dwarf eclipsing binary CM Draconis with TESS: spots, flares, and ultra-precise parameters |journal=[[Monthly Notices of the Royal Astronomical Society]] |volume=528 |issue=1 |pages=963–975 |doi=10.1093/mnras/stae015 |doi-access=free |arxiv=2301.10858 |bibcode=2024MNRAS.528..963M}}</ref><br />(0.25113 ± 0.00016 {{Solar radius|link=y}})
| style="text-align:center;" |{{number sign}}
| data-sort-value="235.8"|235.8 ± 0.3<ref name="Martin2024" /><br />{{nowrap|(0.22507 ± 0.00024 {{Solar mass|link=y}})}}
| One of the lightest stars with precisely measured masses and radii, orbiting around 1.268 days. Age: 4.1 ± 0.8 [[Gigayear|Gyr]].<ref name=":0">{{Cite journal |last1=Morales |first1=Juan Carlos |last2=Ribas |first2=Ignasi |last3=Jordi |first3=Carme |last4=Torres |first4=Guillermo |last5=Gallardo |first5=José |last6=Guinan |first6=Edward F. |last7=Charbonneau |first7=David |last8=Wolf |first8=Marek |last9=Latham |first9=David W. |last10=Anglada-Escudé |first10=Guillem |last11=Bradstreet |first11=David H. |last12=Everett |first12=Mark E. |last13=O'Donovan |first13=Francis T. |last14=Mandushev |first14=Georgi |last15=Mathieu |first15=Robert D. |date=2009-02-01 |title=Absolute Properties of the Low-Mass Eclipsing Binary Cm Draconis |url=https://iopscience.iop.org/article/10.1088/0004-637X/691/2/1400 |journal=The Astrophysical Journal |volume=691 |issue=2 |pages=1400–1411 |arxiv=0810.1541 |bibcode=2009ApJ...691.1400M |doi=10.1088/0004-637X/691/2/1400 |issn=0004-637X}}</ref><br /><small>''Reported for reference.''</small>
|- style="background:#FFF8DC"
| style="border:4px ridge purple; background:white; text-align:center |[[File:PZTelLightCurve.png|112x112px]]
| [[PZ Telescopii|PZ Telescopii b]]<br />''(PZ Tel b,<br />HD 174429 b)''
| 2.42 {{±|0.28|0.34}}<ref>{{Cite journal |last1=Schmidt |first1=T. O. B. |last2=Mugrauer |first2=M. |last3=Neuhäuser |first3=R. |last4=Vogt |first4=N. |last5=Witte |first5=S. |last6=Hauschildt |first6=P. H. |last7=Helling |first7=Ch. |last8=Seifahrt |first8=A. |date=June 2014 |title=First spectroscopic observations of the substellar companion of the young debris disk star PZ Telescopii |url=http://www.aanda.org/10.1051/0004-6361/201321625 |journal=Astronomy & Astrophysics |volume=566 |pages=A85 |arxiv=1404.2870 |bibcode=2014A&A...566A..85S |doi=10.1051/0004-6361/201321625 |issn=0004-6361}}</ref>
| style="text-align:center;" |{{asterisk}}
| 27 {{±|25|9}}<ref>{{Cite journal |last1=Franson |first1=Kyle |last2=Bowler |first2=Brendan P. |date=2023-06-01 |title=Dynamical Mass of the Young Brown Dwarf Companion PZ Tel B |journal=The Astronomical Journal |volume=165 |issue=6 |pages=246 |arxiv=2304.01302 |bibcode=2023AJ....165..246F |doi=10.3847/1538-3881/acca18 |doi-access=free |issn=0004-6256}}</ref>
| Likely a brown dwarf. First possible extra Jupiter-like planet to be directly imaged<ref name="Jenkins 2012">{{cite journal |last1=Jenkins |first1=J. S. |last2=Pavlenko |first2=Y. V. |last3=Ivanyuk |first3=O. |last4=Gallardo |first4=J. |last5=Jones |first5=M. I. |last6=Day-Jones |first6=A. C. |last7=Jones |first7=H. R. A. |last8=Ruiz |first8=M. T. |last9=Pinfield |first9=D. J. |last10=Yakovina |first10=L. |title=Benchmark Cool Companions: Ages and Abundances for the PZ Telescopii System |display-authors=4 |journal=Monthly Notices of the Royal Astronomical Society |volume=420 |issue=4 |pages=3587–98  |date=2012
 |bibcode=2012MNRAS.420.3587J |arxiv=1111.7001 |doi=10.1111/j.1365-2966.2011.20280.x |doi-access=free |s2cid=18735984}}</ref>
|- style="background:pink;"
| style="border:4px ridge purple; background:white; text-align:center |[[File:CMDraLightCurve.png|112x112px]]
| [[CM Draconis|CM Draconis B]]<br />''(Gliese 630.1 Ab)''
| data-sort-value="2.3094"|2.3094 ± 0.0001<ref name="Martin2024" /><br />(0.23732 ± 0.00014 {{Solar radius|link=y}})
| style="text-align:center;" |{{number sign}}
| data-sort-value="220.2"|220.2 ± 0.3<ref name="Martin2024" /><br />(0.21017 ± 0.00028 {{Solar mass|link=y}})
|One of the lightest stars with precisely measured masses and radii, orbiting around 1.268 days. Age: 4.1 ± 0.8 [[Gigayear|Gyr]].<ref name=":0" /><br /><small>''Reported for reference.''</small>
|- style="background:#FFE8DC"
|
| [[o005 s41280]] 
| data-sort-value="2.30"|2.30<ref name="Tu2025">{{Cite arXiv |eprint=2501.16648 |last1=Tu |first1=Zhijun |last2=Wang |first2=Shu |last3=Chen |first3=Xiaodian |last4=Liu |first4=Jifeng |title=Three Brown Dwarfs Masquerading as High-Redshift Galaxies in JWST Observations |date=2025 |class=astro-ph.SR }}</ref>
| style="text-align:center;" |{{dagger}}
| data-sort-value="8.4"|8.4<ref name="Tu2025"/> 
| May be a [[sub-brown dwarf]] or a [[rogue planet]]<ref name="Tu2025"/>
|- style="background:#FFE8DC"
|
| [[TWA 29]] 
| data-sort-value="2.222"|2.222 {{±|0.082|0.081}}<ref name="Hurt-2024" />
| style="text-align:center;" |{{dagger}}
| data-sort-value="6.6"|6.6 {{±|5.2|2.9}}<ref name="Hurt-2024" />
| [[Rogue planet]]
|- style="background:#e6e6e6" 
|style="border:4px ridge red; background:#000000; text-align:center;"|[[File:Artist’s impression of an ultra-hot Jupiter transiting its star.jpg|112x112px]]
| ''[[Hot Jupiter]] limit''
| data-sort-value="2.2"|2.2<ref name="limit" />
| style="text-align:center;" |–
| data-sort-value="0.0000000000000000001"|> 0
| Theoretical limit for [[hot Jupiter]]s close to a star, that are limited by [[tidal heating]], resulting in 'runaway inflation'
|-
| style="border:4px ridge orange; background:#000000;" |[[File:Comparison XO-6.png|112x112px]]
| [[XO-6b]] 
| data-sort-value="2.17" |2.17 ± 0.2<ref name="Saha2024" />
| style="text-align:center;" |←
| data-sort-value="4.47" |4.47 ± 0.12<ref name="Saha2024" />
| A very puffy [[Hot Jupiter]]
|- style="background:#FFE8DC"
|
| [[PSO J077.1+24]] 
| data-sort-value="2.14"|2.14<ref name=":17" />{{efn|name=L/Teff|Based on the estimated temperature and luminosity via the [[Stefan-Boltzmann law]].}}
| style="text-align:center;" |{{dagger}}
| data-sort-value="5.9"|5.9 {{±|0.9|0.8}}<ref name=":17" /> 
| [[Rogue planet]]
|- style="background:#FFE8DC"
|
| [[CAHA Tau 1]]
| data-sort-value="2.12"|2.12<ref name="Quanz-2010" /><ref name="Encyclopaedia of exoplanetary systems / exoplanet.eu">{{Cite web |title=Planet CAHA Tau 1 |url=https://exoplanet.eu/catalog/caha_tau_1--9138/ |access-date=9 September 2024 |website=Encyclopaedia of exoplanetary systems / exoplanet.eu}}</ref>{{efn|name=L/Teff|Based on the estimated temperature and luminosity via the [[Stefan-Boltzmann law]].}}
| style="text-align:center;" |{{dagger}}
| data-sort-value="10.001"|10 ± 5<ref name="Quanz-2010" /><ref name="Encyclopaedia of exoplanetary systems / exoplanet.eu" />
| [[Rogue planet]]
|-
|style="border:4px ridge blue; background:#000000; text-align:center;"|[[File:ROXs 42B MUSE IR.jpg|112x112px]]
| [[ROXs 42Bb|ROXs 42B b]]
| data-sort-value="2.105"|2.10 ± 0.35<ref name="Xuan-2024" /> 
| style="text-align:center;" |←
| data-sort-value="9"|9 {{±|6|3}},<ref name=":12" /> 10 ± 4<ref name=":13" />
| Older estimates include 1.9 – 2.4, 1.3{{Snd}}4.7 {{Jupiter radius|link=y}}<ref name="DaemgenROX" /> and 2.43{{±|0.18}}, 2.55{{±|0.2}} {{Jupiter radius|link=y}}.<ref name=":14" /> Other recent sources of masses include 3.2 – 27 {{Jupiter mass|link=y}},<ref name="Inglis2024" /> 13 ± 5 {{Jupiter mass|link=y}}.<ref name="Xuan-2024" />
|-
| style="border:4px ridge purple; background:white; text-align:center |[[File:Transit light curve of Hat-P-67b.png|112x112px]]
| [[HAT-P-67b]]
| data-sort-value="2.038"|2.038 {{±|0.068|0.038}},<ref name=Saha2024 /><br />2.165 {{±|0.024|0.022}}{{efn|name=HatP67|Calculated using R<sub>p</sub>/R<sub>⋆</sub> multiplied by R<sub>⋆</sub>. The value is later multiplied by (142984 ''km'' ÷ 1391400 ''km'') to convert from {{solar radius|link=y}} to {{jupiter radius|link=y}}.}}<ref name=Gully-Santiago />
| style="text-align:center;" |←
| data-sort-value="0.418"|0.418 ± 0.012<ref name=Saha2024 />
| A very puffy [[Hot Jupiter]]. Was the largest known planet with an accurately and precisely measured radius<ref name="largest" /> (2.085 {{±|0.096|0.071}} {{Jupiter radius|link=y}}),<ref name="Zhou2017HAT" /> until a new estimate revised its radius in 2024.<ref name=Gully-Santiago /><ref name=Saha2024 />
|-
|
| [[HATS-15b]]
| data-sort-value="2.019"|2.019 {{±|0.202|0.160}}<ref name="Johns" />
| style="text-align:center;" |←
| data-sort-value="2.17"|2.17 ± 0.15<ref name="Johns" />
|
|- style="background:#FFE8DC"
|style="border:4px ridge blue; background:#000000; text-align:center;"| [[File:WISE1109-7734 (with marker, edited).png|112x112px]]
| [[Cha 110913-773444]]<br />''(Cha 110913)''
| data-sort-value="2.005"|2.0{{snd}}2.1<ref name="Bonnefoy-2014" />
| style="text-align:center;" |{{dagger}}
| data-sort-value="8.001"|8 {{±|7|3}}<ref name="IM4rM" />
| 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.<ref name="Bonnefoy-2014" />
|- style="background:#FFE8DC"
|
| [[CFHTWIR-Oph 90]]<br />''(Oph 90)''
| data-sort-value="2.001"|2.00 {{±|0.09|0.12}};<ref name="Bryan-2020" /><br /> 3<ref name="rilinger" /><ref name="l7XWJ" />
| style="text-align:center;" |{{dagger}}
| data-sort-value="10.501"|10.5<ref name="rilinger" />
| May be [[rogue planet]] or [[brown dwarf]]
|- style="background:#FFE8DC"
|
| [[SSTB213 J041757|SSTB213 J041757 A]]
| data-sort-value="2"|2<ref name="ReferenceA">{{Cite EPE|name=SSTB213 J041757|id=9834}}</ref>
| style="text-align:center;" |{{dagger}}
| data-sort-value="3.5"|3.5<ref name="ReferenceA" />
| In a binary with a smaller {{Jupiter radius|1.7}} [[#SSTB213 J041757b|planet]].

|-
|style="border:4px ridge red; background:#000000; text-align:center;"|[[File:Kepler-435b.png|112x112px]]
| [[Kepler-435b]]<br />''(KOI-614 b)''
| data-sort-value="1.99"|1.99 ± 0.18<ref name="Almenara-2015" />
| style="text-align:center;" |←
| data-sort-value="0.84"|0.84 ± 0.15<ref name="Almenara-2015" />
|
|-
| style="border:4px ridge blue; background:#000000; text-align:center;" |[[File:PDS 70 closeup - eso2111a.jpg|112x112px]]
| [[PDS 70 c]]
| data-sort-value="1.98" |1.98 {{±|0.39|0.31}}<ref name="Wang2021" />
| style="text-align:center;" |←
| data-sort-value="7.5" |7.5 {{±|4.7|4.2}}, {{nowrap|7.8 {{±|5.0|4.7}}}}, {{nowrap|~1 − ~15}} (total)<ref name="Wang 王-2021" />
| 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]]).<ref name="fdieh" /> PDS 70 is the second multi-[[planetary system|planet system]] to be directly imaged (after [[HR 8799#Planetary system|HR 8799]]). 
|-
|style="border:4px ridge blue; background:#000000; text-align:center;"|[[File:PDS 70.jpg|112x112px]]
| [[PDS 70 b]]
| data-sort-value="1.96"|1.96 {{±|0.20|0.17}}<ref name="Wang2021" /> 
| style="text-align:center;" |←
| data-sort-value="3.2"|3.2 {{±|3.3|1.6}}, 7.9 {{±|4.9|4.7}}, {{nowrap|< 10 (2 σ)}}, {{nowrap|≲ 15 (total)}}<ref name="Wang 王-2021" />
| First [[protoplanet]] to have been ever detected. PDS 70 is the second [[List of multiplanetary systems|multiplanetary system]] to be directly imaged (after [[HR 8799#Planetary system|HR 8799 system]]). Other source of radius includes 2.7 {{Jupiter radius|link=y}}.<ref name=Zhou2022 />
|-
| style="border:4px ridge red; background:#000000; text-align:center;"|[[File:Star OGLE2-TR-L9 and planet.png|112px]]
| [[OGLE2-TR-L9b]] 
| data-sort-value="1.958"|{{val|1.958|0.174|0.111}}<ref name="Johns" />
| style="text-align:center;" |←
| data-sort-value="4.5"|{{val|4.5|1.5}}<ref name="Johns" />
| First discovered planet orbiting a fast-rotating hot star, [[OGLE2-TR-L9]].<ref name="disc" />
|- style="background:#FFF8DC"
| style="border:4px ridge blue; background:#000053; text-align:center;" |[[File:CFHTWIR-Oph 98 AB WFC3.jpg|112x112px]]
| [[CFHTWIR-Oph 98|CFHTWIR-Oph 98 A]]
| data-sort-value="1.95"|1.95{{±|0.11|0.10}};<ref name="Bryan-2020" /> 2.14<ref name="rilinger" /><ref name="Encyclopaedia of exoplanetary systems / Exoplanet.eu">{{Cite web |title=Planet CFHTWIR-Oph 98 b |url=https://exoplanet.eu/catalog/cfhtwir_oph_98_b--7873/ |access-date=2024-08-15 |website=Encyclopaedia of exoplanetary systems / Exoplanet.eu}}</ref>
| style="text-align:center;" |{{asterisk}}
| data-sort-value="15.4"|15.4 ± 0.8;<ref name="Fontanive-2020" /><br />10.5<ref name="rilinger" /> 
| Either a [[M-type star|M-type]] [[brown dwarf]] or [[sub-brown dwarf]] with a sub-brown dwarf/[[exoplanet|planet]] companion [[CFHTWIR-Oph 98 b]].<br />Other sources of masses includes: 9.6 – 18.4 {{Jupiter mass|link=y}}.<ref name="Fontanive-2020" />
|-
|
| [[WASP-178b]]<br />''(KELT-26 b,<br />HD 134004 b)''
| data-sort-value="1.940"|1.940 {{±|0.060|0.058}}<ref name="Martínez-2020" />
| style="text-align:center;" |←
| data-sort-value="1.41"|1.41 {{±|0.43|0.51}}<ref name="Martínez-2020" />
| An [[Hot Jupiter|ultra-hot Jupiter]]. Initially, the planet's atmosphere was discovered having [[silicon monoxide]], making this exoplanet the first one to have the [[chemical compound|compound]] on its atmosphere,<ref name="Lothringer2022" /> now the atmosphere is more likely dominated by [[ionized]] [[magnesium]] and [[iron]].<ref name="Damasceno2024" />
|-
|style="border:4px ridge red; background:#000000; text-align:center;"| [[File:WASP-12b a Hot, Carbon-Rich Planet.jpg|112x112px]]<!-- Do not change, this is an accurate illustration, since WASP-12b is highly irradiated and bright, it would appear as orangish due to its blackbody radiation, rather than purely black. -->
| [[WASP-12b|WASP-12Ab]]
| data-sort-value="1.937"|1.937 ± 0.056<ref name="WRrrL" /> 
| style="text-align:center;" |←
| data-sort-value="1.476"|1.47 {{±|0.076|0.069}}<ref name="collins" />
| This planet is so close to [[WASP-12|WASP-12 A]] that its tidal forces are distorting it into an [[ellipsoid|egg-like shape]].<ref>{{Cite journal |first1=Shu-lin |last1=Li |first2=N. |last2=Miller |first3=Douglas N. C. |last3=Lin |name-list-style=amp |first4=Jonathan J. |last4=Fortney |date=2010 |title=WASP-12b as a prolate, inflated and disrupting planet from tidal dissipation |journal=[[Nature (journal)|Nature]] |volume=463 |issue=7284 |pages=1054–1056 |doi=10.1038/nature08715 |pmid=20182506 |bibcode = 2010Natur.463.1054L |arxiv = 1002.4608 |s2cid=4414948}}</ref> First planet observed being consumed by its host star;<ref name="Hubble observation">[http://www.nasa.gov/mission_pages/hubble/science/planet-eater.html Hubble Finds a Star Eating a Planet] nasa.gov. 2010-05-20. Retrieved on 2010-12-10.</ref> it will be destroyed in 3.16 ± 0.10 {{val|ul=Myr}} due to [[tidal force|tidal interactions]].<ref>{{Cite web |last=waspplanets |date=2019-11-26 |title=The orbit of WASP-12b is decaying |url=https://wasp-planets.net/2019/11/26/the-orbit-of-wasp-12b-is-decaying/ |access-date=2020-01-01 |website=WASP Planets |language=en}}</ref><ref>{{cite journal |last1=Wong |first1=Ian |last2=Shporer |first2=Avi |last3=Vissapragada |first3=Shreyas |last4=Greklek-McKeon |first4=Michael |last5=Knutson |first5=Heather A. |last6=Winn |first6=Joshua N. |last7=Benneke |first7=Björn |date=20 January 2022 |title=TESS Revisits WASP-12: Updated Orbital Decay Rate and Constraints on Atmospheric Variability |journal=The Astronomical Journal |volume=163 |issue=4 |page=175 |arxiv=2201.08370 |bibcode=2022AJ....163..175W |doi=10.3847/1538-3881/ac5680 |s2cid=246063389 |doi-access=free}}</ref><br />WASP-12b is suspected to have [[WASP-12b#Candidate satellite|one exomoon]] due to a curve of change of shine of the planet observed regular variation of light.<ref name="EytJY" />
|-style="background:#FFF8DC"
|
| [[BD-14 3065 b]]<br />''(TOI-4987 b)''
| data-sort-value="1.926"|1.926 ± 0.094<ref name="Šubjak-2024" />
| style="text-align:center;" |{{asterisk}}
| data-sort-value="12.37"|12.37 ± 0.92<ref name="Šubjak-2024" />
| Might be a [[brown dwarf]] fusing [[deuterium]] at its core, which could explain its anomalous high radius. Also [[List of hottest exoplanets|one of the hottest known exoplanets]], measuring {{Convert|3520|K|C F}}.<ref name="Šubjak-2024" />
|-
|style="border:4px ridge red; background:#000000; text-align:center;"|[[File:PIA21472 - Hottest Hot Jupiter Animation (Artist's Concept).gif|112x112px]]
| [[KELT-9b]]<br />''(HD 195689 b)''
| data-sort-value="1.891"|1.891 {{±|0.061|0.055}}<ref name="lNqlN" />
| style="text-align:center;" |←
| data-sort-value="2.171"|2.17 ± 0.56<ref name="qYLMK" />
| Hottest confirmed exoplanet, with a temperature of {{val|4050|180|ul=K}} (3777 ± 180 {{val|ul=°C}}; 6830 ± 324 {{val|ul=°F}}).<ref name="scottgaudi" />
|-
|
| [[TOI-1518 b]]
| data-sort-value="1.875"|1.875 ± 0.053<ref name="Cabot-2021" />
| style="text-align:center;" |←
| data-sort-value="2.29999"|< 2.3 (2 σ)<ref name="Cabot-2021" />
|
|-
|
| [[HAT-P-70b]]
| data-sort-value="1.87"|1.87 {{±|0.15|0.10}}<ref name="Zhou-2019" />
| style="text-align:center;" |←
| data-sort-value="6.78"|< 6.78 (3 σ)<ref name="Zhou-2019" />
|
|- style="background:#FFE8DC"
| 
| [[2MASS J1935-2846]]
| data-sort-value="1.869"|1.869 ± 0.053<ref name=":18">{{Cite journal |last1=Hurt |first1=Spencer A. |last2=Liu |first2=Michael C. |last3=Zhang |first3=Zhoujian |last4=Phillips |first4=Mark |last5=Allers |first5=Katelyn N. |last6=Deacon |first6=Niall R. |last7=Aller |first7=Kimberly M. |last8=Best |first8=William M. J. |date=2024-01-01 |title=Uniform Forward-modeling Analysis of Ultracool Dwarfs. III. Late-M and L Dwarfs in Young Moving Groups, the Pleiades, and the Hyades |journal=The Astrophysical Journal |volume=961 |issue=1 |pages=121 |arxiv=2311.04268 |bibcode=2024ApJ...961..121H |doi=10.3847/1538-4357/ad0b12 |doi-access=free |issn=0004-637X}}</ref>
| style="text-align:center;" |{{dagger}}
| data-sort-value="7.4"|7.4 {{±|6.3|3.4}}<ref name=":18" />
| May be a [[sub-brown dwarf]] or [[rogue planet]].
|- style="background:#CEE0F2" 
|
| [[HATS-23b]]
| data-sort-value="1.866"|1.86 {{±|0.30|0.40}}<ref name="Bento-2017" />
| style="text-align:center;" | →
| data-sort-value="1.4702"|1.470 ± 0.072<ref name="Bento-2017" />
|Grazing planet.
|- style="background:#FFE8DC"
| style="border:4px ridge blue; background:#000053; text-align:center;"|[[File:CFHTWIR-Oph 98 AB WFC3.jpg|112x112px]]
| [[CFHTWIR-Oph 98 b]]<br />''(Oph 98 b,<br />CFHTWIR-Oph 98 B)''
| data-sort-value="1.865"|1.86 ± 0.05<ref name="NASAExoplanetArchive" /><ref name="Encyclopaedia of exoplanetary systems / Exoplanet.eu">{{Cite web |title=Planet CFHTWIR-Oph 98 b |url=https://exoplanet.eu/catalog/cfhtwir_oph_98_b--7873/ |access-date=2024-08-15 |website=Encyclopaedia of exoplanetary systems / Exoplanet.eu}}</ref>
| style="text-align:center;" |{{dagger}}
| data-sort-value="7.8"|7.8 {{±|0.7|0.8}}<ref name="Fontanive-2020" />
| Its formation as an exoplanet is challenging or impossible.<ref name="Fontanive2020">{{Cite journal |last1=Fontanive |first1=Clémence |last2=Allers |first2=Katelyn N. |last3=Pantoja |first3=Blake |last4=Biller |first4=Beth |last5=Dubber |first5=Sophie |last6=Zhang |first6=Zhoujian |last7=Dupuy |first7=Trent |last8=Liu |first8=Michael C. |last9=Albert |first9=Loïc |date=2020-12-01 |title=A Wide Planetary-mass Companion to a Young Low-mass Brown Dwarf in Ophiuchus |journal=The Astrophysical Journal |volume=905 |issue=2 |pages=L14 |doi=10.3847/2041-8213/abcaf8 |issn=0004-637X|doi-access=free |arxiv=2011.08871 |bibcode=2020ApJ...905L..14F}}</ref> 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]].<br />Other sources of mass includes 4.1 – 11.6 {{Jupiter mass|link=y}}.<ref name="Fontanive-2020" />
|-
|
| [[KELT-8b]]
| data-sort-value="1.86"|1.86 {{±|0.18|0.16}}<ref name="Fulton-2015" />
| style="text-align:center;" |←
| data-sort-value="0.867"|0.867 {{±|0.065|0.061}}<ref name="Fulton-2015" />
|
|- style="background:#FFE8DC"
|
| [[KPNO-Tau 12]]
| data-sort-value="1.84"|1.84,<ref name="Kraus-2006" /><br />2.22 {{±|0.11|0.17}}<ref name="Bryan-2020" />
| style="text-align:center;" |{{dagger}}
| data-sort-value="11.5"|11.5<ref name="rilinger" />
| A member of Taurus-Auriga star-forming region.<ref name="Kraus-2006" />
|-
| style="border:4px ridge orange; background:#000000; text-align:center;" |[[File:TrES-4.jpg|112x112px]]
| [[TrES-4b|TrES-4]]<br />''(GSC 06200-00648 Ab)''
| data-sort-value="1.838"|1.838 {{±|0.240|0.238}}<ref name="Johns" />
| style="text-align:center;" |←
| data-sort-value="0.78"|0.78 ± 0.19<ref name="Stassun-2017" />
| This planet has a density of 0.17 g/cm<sup>3</sup>,<ref name="Johns" /> about that of [[balsa wood]], less than Saturn's 0.7 g/cm<sup>3</sup>.
|-
|
| [[HAT-P-33b]] 
| data-sort-value="1.827"|1.827 ± 0.29,<ref name="o5qXL" /><br />{{val|1.85|0.49}}<ref name="NASAExoplanetArchive" />
| style="text-align:center;" |←
| data-sort-value="0.72"|0.72 {{±|0.13|0.12}}<ref name="Wang2017" />
|
|-
|
| [[HAT-P-32b]] 
| data-sort-value="1.822"|1.822 {{±|0.350|0.236}}<ref name="Johns" />
| style="text-align:center;" |←
| data-sort-value="0.941"|0.941 ± 0.166,<br />0.860 ± 0.164<ref name="6LQQh" /> 
|
|-
|style="border:4px ridge red; background:#222222; text-align:center"|[[File:UHJ KELT-20b.webp|112px]]
| [[KELT-20b]] <br />''(MASCARA-2b)''
| data-sort-value="1.821"|1.821{{±|0.045}}<ref name=Saha2023 />
| style="text-align:center;" |←
| data-sort-value="3.355"|3.355{{±|0.062|0.063}}<ref name=Saha2023 />
| An [[ultra-hot Jupiter]]. 
|- style="background:#FFF8DC"
|style="border:4px ridge blue; background:#000000; text-align:center;"| [[File:First ever image of a multi-planet system around a Sun-like star.tif|112x112px]]
| [[YSES 1 b]]<br />''(TYC 8998-760-1 b)''
| data-sort-value="1.821"|{{nowrap|1.82 ± 0.08<ref name="vb0fx" />{{snd}}3.0 {{±|0.2|0.7}}<ref name="The Extrasolar Planet Encyclopaedia-1995" />}} 
| style="text-align:center;" |{{asterisk}}
| data-sort-value="21.8"|21.8 ± 3<ref name="Wood-2023" />
| Likely a [[brown dwarf]]. First substellar object to have an [[isotope]] ([[Carbon-13|<sup>13</sup>C]]) in its atmosphere.<ref name="SA-20210714">{{cite news |last=Starr |first=Michelle |title=Isotopes Detected in The Atmosphere of an Exoplanet For The First Time |url=https://www.sciencealert.com/for-the-first-time-isotopes-have-been-detected-in-the-atmosphere-of-an-exoplanet |date=14 July 2021 |work=[[ScienceAlert]] |access-date=14 July 2021}}</ref><ref name="vb0fx" /> First [[direct imaging|directly imaged]] [[planetary system]] having multiple bodies orbiting a Sun-like star.<ref name="ESO_Bohn">{{cite web |last1=ESO/Bohn |title=First ever image of a multi-planet system around a Sun-like star (uncropped, with annotations) |url=https://www.eso.org/public/images/eso2011b/ |website=ESO |publisher=European Southern Observatory |access-date=24 July 2020 |archive-url=https://web.archive.org/web/20200724161316/https://www.eso.org/public/images/eso2011b/ |archive-date=24 July 2020 |date=22 July 2020}}</ref><ref name="Wall">{{cite news |last=Wall |first=Mike |title=Multiplanet system around sunlike star photographed for 1st time ever - The two newly imaged planets are huge — 14 and 6 times more massive than Jupiter. |url=https://www.space.com/multiplanet-system-sun-like-star-first-photo.html |date=22 July 2020 |work=Space.com |access-date=22 July 2020}}</ref>
|- style="background:pink;"
|style="border:4px ridge blue; background:#000000; text-align:center;"|[[File:Barnardstar2006.jpg|112x112px]]
| [[Barnard's Star]] 
| data-sort-value="1.82"|1.82 ± 0.01<ref name="Pineda-2021" /><br />(0.187 ± 0.001 {{val|ul=Solar radius}})
| style="text-align:center;" |{{number sign}}
| data-sort-value="168.7"|168.7 {{±|3.8|3.7}}<ref name="Pineda-2021" /><br />(0.1610 {{±|0.0036|0.0035}} {{val|ul=solar mass}})
| Second nearest [[planetary system]] to the [[Sun]] at the distance of {{cvt|1.83|pc|ly|2|order=flip}} 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.<br />Has a planet, [[Barnard b]] ''(Barnard's Star b)''.<ref name="opzKZ" /><br /><small>''Reported for reference.''</small>
|-
|style="border:4px ridge red; background:#000000; text-align:center;"|[[File:CoRoT-1.jpg|112px]]
| [[CoRoT-1b]]
| data-sort-value="1.805"|1.805 {{±|0.132|0.131}}<ref name="Johns" />
| style="text-align:center;" |←
| data-sort-value="1.03"|1.03 ± 0.12<ref name="Johns" />
| First exoplanet for which optical (as opposed to [[HD 189733 b#Map of the planet|infrared]]) observations of phases were reported.<ref>{{cite journal|title=The changing phases of extrasolar planet CoRoT-1b|journal=Nature|volume= 459|issue=7246|pages=543–545|date=2009-05-28|pmid=19478779|doi=10.1038/nature08045|author1=Ignas A. G. Snellen|author2=Ernst J. W. de Mooij|author3=Simon Albrecht|bibcode = 2009Natur.459..543S |arxiv = 0904.1208 |s2cid=4347612}}</ref>
|-
|
| [[WTS-2b]]
| data-sort-value="1.804"|1.804 {{±|0.144|0.158}}<ref name="Johns" />
| style="text-align:center;" |←
| data-sort-value="1.12"|1.12 ± 0.16<ref name="Johns" />
|
|-
|style="border:4px ridge red; background:#000000; text-align:center;"|[[File:WASP-76 b (2020).png|112x112px]]
| [[WASP-76b]] 
| data-sort-value="1.802"|1.802{{±|0.042}}<ref name=Saha2023 />
| style="text-align:center;" |←
| data-sort-value="0.92"|0.921{{±|0.032}}<ref name=Saha2023 />
|WASP-76b is suspected to have an exomoon analogue to Jupiter's [[Io (moon)|Io]] due to the detection of sodium via [[absorption spectroscopy]].<ref name="Xqd9O" />
|-
| style="border:4px ridge red; background:#000000; text-align:center;" |[[File:UAndAb full.jpg|112x112px]]
| [[Upsilon Andromedae b|Saffar]]<br />''({{nowrap|υ And Ab}})''
| data-sort-value="1.8"|~1.8<ref name="kNo8y" />
| style="text-align:center;" |←
| data-sort-value="1.70"|1.70 {{±|0.33|0.24}}<ref name="s9bfg" />
| Radius estimated using the phase curve of reflected light. The planet orbits very close to [[Upsilon Andromedae A|Titawin]] ''(υ And A)'' at the distance of 0.0595 [[Astronomical unit|AU]], completing an orbit in 4.617 [[day]]s.<ref name="9JjuK" /> First multiple-[[planetary system|planet system]] to be discovered around a [[main-sequence]] star, and first multiple-planet system known in a multiple-[[star system]].
|-
|
| [[HAT-P-40b]]
| data-sort-value="1.799"|1.799 {{±|0.237|0.260}}<ref name="Johns" />
| style="text-align:center;" |←
| data-sort-value="0.48"|0.48 ± 0.13<ref name="Johns" />
| A very puffy hot Jupiter
|-
|
| [[WASP-122b]]<br />''(KELT-14b)''
| data-sort-value="1.795"|1.795 {{±|0.107|0.079}}<ref name="Johns" />
| style="text-align:center;" |←
| data-sort-value="1.284"|1.284 ± 0.032<ref name="Turner-2016">{{Cite journal |last1=Turner |first1=O. D. |last2=Anderson |first2=D. R. |last3=Cameron |first3=A. Collier |last4=Delrez |first4=L. |last5=Evans |first5=D. F. |last6=Gillon |first6=M. |last7=Hellier |first7=C. |last8=Jehin |first8=E. |last9=Lendl |first9=M. |last10=Maxted |first10=P. F. L. |last11=Pepe |first11=F. |last12=Pollacco |first12=D. |last13=Queloz |first13=D. |last14=Ségransan |first14=D. |last15=Smalley |first15=B. |date=2016-06-01 |title=WASP-120 b, WASP-122 b, and WASP-123 b: Three Newly Discovered Planets from the WASP-South Survey |url=https://iopscience.iop.org/article/10.1088/1538-3873/128/964/064401 |journal=Publications of the Astronomical Society of the Pacific |volume=128 |issue=964 |page=064401 |arxiv=1509.02210 |bibcode=2016PASP..128f4401T |doi=10.1088/1538-3873/128/964/064401 |hdl=10023/10795 |issn=0004-6280}}</ref>
|
|-
|
| [[KELT-12b]]
| data-sort-value="1.79"|1.79 {{±|0.18|0.17}}<ref name="Stevens-2017" />
| style="text-align:center;" |←
| data-sort-value="0.95"|0.95 ± 0.14<ref name="Stevens-2017" />
|
|-
|style="border:4px ridge red; background:#000000; text-align:center;"|[[File:WASP-121b 01.jpg|112x112px]]
| [[WASP-121b|Tylos]] <br />''(WASP-121b)''
| data-sort-value="1.773"|1.773 {{±|0.041|0.033}}<ref name=Bourrier2020 />
| style="text-align:center;" |←
| data-sort-value="1.157"|1.157 ± 0.07<ref name=Bourrier2020 />
| First exoplanet found to contain water on its [[stratosphere]]. Tylos is suspected to have an exomoon analogous to Jupiter's [[Io (moon)|Io]] due to the detection of sodium [[absorption spectroscopy]] around it.<ref name="Hoeijmakers2020" />
|-
|
| [[TOI-640 b|TOI-640 Ab]]
| data-sort-value="1.771"|1.771 {{±|0.060|0.056}}<ref name="Rodriguez-2021" />
| style="text-align:center;" |←
| data-sort-value="0.88"|0.88 ± 0.16<ref name="Rodriguez-2021" />
| 
|-
|
| [[WASP-187b]]
| data-sort-value="1.766"|1.766 ± 0.036<ref name=Saha2024 />
| style="text-align:center;" |←
| data-sort-value="0.801"|0.801 {{±|0.084|0.083}}<ref name=Saha2024 />
|
|-
|
| [[WASP-94 Ab]]
| data-sort-value="1.761"|1.761 {{±|0.194|0.191}}<ref name="Johns" />
| style="text-align:center;" |←
| data-sort-value="0.5"|{{val|0.5|0.13}}<ref name="Johns" />
|
|-
|
| [[TOI-2669b]]
| data-sort-value="1.76"|1.76 ± 0.16<ref name="Grunblatt-2022" />
| style="text-align:center;" |←
| data-sort-value="0.61"|0.61 ± 0.19<ref name="Grunblatt-2022" />
|
|- style="background:#FFE8DC"
|
| [[WISE J0528+0901]]
| data-sort-value="1.752"|1.752 {{±|0.292|0.195}}<ref name=":19">{{Cite journal |last1=Burgasser |first1=Adam J. |last2=Lopez |first2=Mike A. |last3=Mamajek |first3=Eric E. |last4=Gagné |first4=Jonathan |last5=Faherty |first5=Jacqueline K. |last6=Tallis |first6=Melisa |last7=Choban |first7=Caleb |last8=Tamiya |first8=Tomoki |last9=Escala |first9=Ivanna |last10=Aganze |first10=Christian |date=2016-03-20 |title=THE FIRST BROWN DWARF/PLANETARY-MASS OBJECT IN THE 32 ORIONIS GROUP* |journal=The Astrophysical Journal |volume=820 |issue=1 |pages=32 |arxiv=1602.03022 |bibcode=2016ApJ...820...32B |doi=10.3847/0004-637X/820/1/32 |doi-access=free |issn=0004-637X}}</ref>
| style="text-align:center;" |{{dagger}}
| data-sort-value="13.001"|13 {{±|3|6}}<ref name=":19" />
|[[Brown dwarf]] or [[rogue planet]].
|-
|
| [[HATS-26b]]
| data-sort-value="1.75"|1.75 ± 0.21<ref name="Espinoza-2016" />
| style="text-align:center;" |←
| data-sort-value="0.650"|0.650 ± 0.076<ref name="Espinoza-2016" />
|
|-
|
| [[Kepler-12b]] 
| data-sort-value="1.7454"|1.7454 {{±|0.076|0.072}}<ref name="Berger-2018" />
| style="text-align:center;" |←
| data-sort-value="0.431"|0.431 ± 0.041<ref name="Fortney-2011" />
| Least-irradiated of four [[Hot Jupiters]] at the time of discovery
|-
|
| [[HAT-P-65b]] 
| data-sort-value="1.744"|1.744 {{±|0.165|0.215}}<ref name=Johns />
| style="text-align:center;" |←
| data-sort-value="0.527"|0.527 ± 0.083<ref name="Hartman-2016" />
| This planet has been suffering [[orbital decay]] due to its close proximity to [[HAT-P-65]]; 0.04 AU.<ref>{{Cite journal|last1=Alvarado-Montes|first1=Jaime A|last2=García-Carmona|first2=Carolina|date=2019-07-01|title=Orbital decay of short-period gas giants under evolving tides|url=https://academic.oup.com/mnras/article/486/3/3963/5470968|journal=Monthly Notices of the Royal Astronomical Society|language=en|volume=486|issue=3|pages=3963–3974|doi=10.1093/mnras/stz1081|doi-access=free |issn=0035-8711|arxiv=1904.07596}}</ref>
|- style="background:#FFE8DC"
| 
| [[2MASS J2352-1100]]
| data-sort-value="1.742"|1.742 {{±|0.035|0.036}}<ref name=":18" />
| style= "text-align:center;" |{{dagger}}
| data-sort-value="12.4"|12.4 {{±|9.4|5.5}}<ref name=":18" />
| [[Brown dwarf]] or [[rogue planet]].
|- 
|
| [[KELT-15b]]
| data-sort-value="1.741"|1.74 ± 0.20<ref name="Stassun-2017" />
| style="text-align:center;" |←
| data-sort-value="1.31"|1.31 ± 0.43<ref name="Stassun-2017" />
|
|-
|
| [[HAT-P-57b]]
| data-sort-value="1.74"|1.74 ± 0.36<ref name="Stassun-2017" />
| style="text-align:center;" |←
| data-sort-value="1.4101"|1.41 ± 1.52<ref name="Stassun-2017" />
|
|-
|
| [[WASP-93b]]
| data-sort-value="1.737"|1.737 {{±|0.121|0.170}}<ref name="Johns" />
| style="text-align:center;" |←
| data-sort-value="1.47"|1.47 ± 0.29<ref name=Johns />
|
|-
|
| [[WASP-82b]]
| data-sort-value="1.726"|{{val|1.726|0.163|0.195}}<ref name=Johns />
| style="text-align:center;" |←
| data-sort-value="1.17"|{{val|1.17|0.20}}<ref name=Johns />
|
|-
|style="border:4px ridge red; background:#000000; text-align:center;"| [[File:WASP-17b.jpg|112x112px]]
| [[WASP-17b|Ditsö̀]] <br />''(WASP-17b)''
| data-sort-value="1.720"|1.720 {{±|0.004|0.005}},<br />1.83 ± 0.01<ref name=Grant2024>{{Cite journal |last1=Grant |first1=David |last2=Lewis |first2=Nikole K. |last3=Wakeford |first3=Hannah R. |last4=Batalha |first4=Natasha E. |last5=Glidden |first5=Ana |last6=Goyal |first6=Jayesh |last7=Mullens |first7=Elijah |last8=MacDonald |first8=Ryan J. |last9=May |first9=Erin M. |last10=Seager |first10=Sara |last11=Stevenson |first11=Kevin B. |last12=Valenti |first12=Jeff A. |last13=Visscher |first13=Channon |last14=Alderson |first14=Lili |last15=Allen |first15=Natalie H. |date=2023-10-01 |title=JWST-TST DREAMS: Quartz Clouds in the Atmosphere of WASP-17b |journal=The Astrophysical Journal Letters |volume=956 |issue=2 |pages=L32 |doi=10.3847/2041-8213/acfc3b |doi-access=free |arxiv=2310.08637 |bibcode=2023ApJ...956L..32G |issn=2041-8205}}</ref>
| style="text-align:center;" |←
| data-sort-value="0.512"|0.512 ± 0.037<ref name="Bonomo-2017b" />
| First planet discovered to have a [[retrograde orbit]]<ref name="Anderson2010">{{cite journal | title=WASP-17b: An Ultra-Low Density Planet in a Probable Retrograde Orbit | last1=Anderson | first1=D. R. | last2=Hellier | first2=C. | last3=Gillon | first3=M. | last4=Triaud | first4=A. H. M. J. | last5=Smalley | first5=B. | last6=Hebb | first6=L. | last7=Collier Cameron | first7=A. | last8=Maxted | first8=P. F. L. | last9=Queloz | first9=D. | last10=West | first10=R. G. | last11=Bentley | first11=S. J. | last12=Enoch | first12=B. | last13=Horne | first13=K. | last14=Lister | first14=T. A. | last15=Mayor | first15=M. | last16=Parley | first16=N. R. | last17=Pepe | first17=F. | last18=Pollacco | first18=D. | last19=Ségransan | first19=D. | last20=Udry | first20=S. | last21=Wilson | first21=D. M. | display-authors=1 | journal=The Astrophysical Journal | volume=709 | issue=1 | pages=159–167 | year=2010 | arxiv=0908.1553 | bibcode=2010ApJ...709..159A | doi=10.1088/0004-637X/709/1/159 | s2cid=53628741}}</ref> and first to have [[quartz]] (crystalline silica, SiO<sub>2</sub>) in its clouds.<ref name="Quartz">{{cite news |url=https://esawebb.org/images/WASP17b/ |title=Composition of cloud particles - hot gas giant exoplanet WASP-17b. |date=October 20, 2023}}</ref> {{nowrap|Has an exteremely low density of 0.08 {{val|ul=g/cm3}}}},<ref name=":3" /> the lowest of any exoplanet when it was discovered, and was possibly the largest exoplanet at the time of discovery, with a radius of {{Jupiter radius|1.92|link=y}}.<ref name="BP" /> 
|-
|
| [[KELT-19 Ab]]
| data-sort-value="1.717"|1.717{{±|0.094|0.093}}<ref name=Saha2023 />
| style="text-align:center;" |←
| data-sort-value="3.98"|3.98{{±|0.32|0.33}}<ref name=Saha2023 />
|
|-
|
| [[HAT-P-39b]]
| data-sort-value="1.712"|{{val|1.712|0.140|0.115}}<ref name=Johns />
| style="text-align:center;" |←
| data-sort-value="0.599"|{{val|0.60|0.10}}<ref name=Johns />
|
|-
|
| [[KELT-4Ab]] 
| data-sort-value="1.706" |1.706 {{±|0.085|0.076}}<ref name="KELT-4Ab" />
| style="text-align:center;" |←
| data-sort-value="0.878" |0.878 {{±|0.070|0.067}}<ref name="KELT-4Ab" />
|
|-
|
| [[WASP-79b|Pollera]]<br />''(WASP-79b)''
| data-sort-value="1.704"|1.704 {{±|0.195|0.180}}<ref name="Johns" />
| style="text-align:center;" |←
| data-sort-value="0.850"|0.850 {{±|0.180|0.180}}<ref name="Johns" />
|
|-
|
| [[HAT-P-64b]]
| data-sort-value="1.703"|1.703 ± 0.070<ref name="Bakos-2021" />
| style="text-align:center;" |←
| data-sort-value="0.58"|0.58 {{±|0.18|0.13}}<ref name="Bakos-2021" />
|
|-
|
| [[WASP-78b]]
| data-sort-value="1.702"|1.70 ± 0.04,<ref name="wasp7879" /> <br />1.93 ± 0.45<ref name="NASAExoplanetArchive" />
| style="text-align:center;" |←
| data-sort-value="0.89"|0.89 ± 0.08<ref name="wasp7879" />
| This planet has likely undergone in the past a migration from the initial highly eccentric orbit.<ref name="arN27" />
|-
|
| [[Qatar-7b]]
| data-sort-value="1.701"|1.70 ± 0.03<ref name="NASAExoplanetArchive" />
| style="text-align:center;" |←
| data-sort-value="1.88"|1.88 ± 0.25<ref name="hZi7q" />
| 
|- style="background:#FFE8DC"
|
| [[SSTB213 J041757 b]]
| data-sort-value="1.70"|1.70<ref name="ReferenceB">{{Cite EPE|name=SSTB213 J041757 b|id=9835}}</ref>
| style="text-align:center;" |{{dagger}}
| data-sort-value="1.50"|1.50<ref name="ReferenceB"/>
| In a binary with a larger {{Jupiter radius|2}} [[#SSTB213 J041757 a|planet]].
|-
|
| [[CoRoT-17b]]
| data-sort-value="1.694" |1.694 {{±|0.139|0.193}}<ref name="Johns"/>
| style="text-align:center;" |←
| data-sort-value="2.430" |2.430{{±|0.300}}<ref name="Johns"/>
|
|-
|
| [[TOI-615b]]
| data-sort-value="1.69"|1.69{{±|0.06|0.05}}<ref name=":2">{{Cite journal |last1=Psaridi |first1=Angelica |last2=Bouchy |first2=François |last3=Lendl |first3=Monika |last4=Akinsanmi |first4=Babatunde |last5=Stassun |first5=Keivan G. |last6=Smalley |first6=Barry |last7=Armstrong |first7=David J. |last8=Howard |first8=Saburo |last9=Ulmer-Moll |first9=Solène |last10=Grieves |first10=Nolan |last11=Barkaoui |first11=Khalid |last12=Rodriguez |first12=Joseph E. |last13=Bryant |first13=Edward M. |last14=Suárez |first14=Olga |last15=Guillot |first15=Tristan |date=2023-07-01 |title=Three Saturn-mass planets transiting F-type stars revealed with TESS and HARPS: TOI-615b, TOI-622b, and TOI-2641b |url=https://ui.adsabs.harvard.edu/abs/2023A&A...675A..39P/abstract |journal=Astronomy and Astrophysics |volume=675 |pages=A39 |doi=10.1051/0004-6361/202346406 |arxiv=2303.15080 |bibcode=2023A&A...675A..39P |issn=0004-6361}}</ref>
|style="text-align:center;"|←
| data-sort-value="0.43"|0.43{{±|0.09|0.08}}<ref name=":2"/>
|
|-
|
| [[TOI-1855 b]]
| data-sort-value="1.65"|1.65 {{±|0.52|0.37}}<ref name="Jack20244">{{cite journal |mode=cs2 |last1=Schulte |first1=Jack |title=Migration and Evolution of giant ExoPlanets (MEEP) I: Nine Newly Confirmed Hot Jupiters from the TESS Mission |date=2024-01-11 |last2=Rodriguez |first2=Joseph E. |last3=Bieryla |first3=Allyson |last4=Quinn |first4=Samuel N. |last5=Collins |first5=Karen A. |last6=Yee |first6=Samuel W. |last7=Nine |first7=Andrew C. |last8=Soares-Furtado |first8=Melinda |last9=Latham |first9=David W.|journal=The Astronomical Journal |volume=168 |issue=1 |page=32 |doi=10.3847/1538-3881/ad4a57 |doi-access=free |arxiv=2401.05923 |bibcode=2024AJ....168...32S }}</ref>
|style="text-align:center;"|←
| data-sort-value="1.133"|1.133 ± 0.096<ref name="Jack20244"/>
| 
|- style="background:#CEE0F2" 
|
| [[TOI-3807 b]]
| data-sort-value="1.6499" |>1.65 (95% lower limit)<ref name="Yee-2023"/>
| style="text-align:center;" | →
| data-sort-value="1.04" |1.04 {{±|0.15|0.14}}<ref name="Yee-2023"/>
| Grazing planet, a large radius of {{jupiter radius|2.00}} derived from transit data is unreliable due to its grazing nature.
|-
|
| [[NGTS-33 b]]
| data-sort-value="1.64"|1.64 ± 0.07<ref name="Douglas2024">{{cite journal |last1=Alves |first1=Douglas R. |last2=Jenkins |first2=James S. |last3=Vines |first3=Jose I. |last4=Battley |first4=Matthew P. |last5=Lendl |first5=Monika |last6=Bouchy |first6=François |last7=Nielsen |first7=Louise D. |last8=Gill |first8=Samuel |last9=Moyano |first9=Maximiliano |last10=Anderson |first10=D. R. |last11=Burleigh |first11=Matthew R. |last12=Casewell |first12=Sarah L. |last13=Goad |first13=Michael R. |last14=Hawthorn |first14=Faith |last15=Kendall |first15=Alicia |last16=McCormac |first16=James |last17=Osborn |first17=Ares |last18=Smith |first18=Alexis M. S. |last19=Udry |first19=Stéphane |last20=Wheatley |first20=Peter J. |last21=Saha |first21=Suman |last22=Parc |first22=Léna |last23=Nigioni |first23=Arianna |last24=Apergis |first24=Ioannis |last25=Ramsay |first25=Gavin |title=NGTS-33b: A Young Super-Jupiter Hosted by a Fast Rotating Massive Hot Star |journal=Monthly Notices of the Royal Astronomical Society |date=2024-11-13 |volume=536 |issue=2 |pages=1538–1554 |doi=10.1093/mnras/stae2582 |doi-access=free |arxiv=2411.08960 |bibcode=2025MNRAS.536.1538A}}</ref>
|style="text-align:center;"|←
| data-sort-value="3.6"|3.6 ± 0.3<ref name="Douglas2024"/>
| 
|-
|
| [[KELT-8b]]
| data-sort-value="1.62"|1.62 ± 0.10<ref name="Stassun-2017" />
|style="text-align:center;"|←
| data-sort-value="0.66"|0.66 ± 0.12<ref name="Stassun-2017" />
| 
|-
|
| [[WASP-82b]]
| data-sort-value="1.62"|1.62 ± 0.13
|style="text-align:center;"|←
| data-sort-value="1.17"|1.17 ± 0.20<ref name="Stassun-2017" />
| 
|-
|
| [[WASP-189 b]]
| data-sort-value="1.619"|1.619 ± 0.021<ref name=":20">{{Cite journal |last1=Lendl |first1=M. |last2=Csizmadia |first2=Sz. |last3=Deline |first3=A. |last4=Fossati |first4=L. |last5=Kitzmann |first5=D. |last6=Heng |first6=K. |last7=Hoyer |first7=S. |last8=Salmon |first8=S. |last9=Benz |first9=W. |last10=Broeg |first10=C. |last11=Ehrenreich |first11=D. |last12=Fortier |first12=A. |last13=Queloz |first13=D. |last14=Bonfanti |first14=A. |last15=Brandeker |first15=A. |date=2020-11-01 |title=The hot dayside and asymmetric transit of WASP-189 b seen by CHEOPS |url=https://ui.adsabs.harvard.edu/abs/2020A&A...643A..94L/abstract |journal=Astronomy and Astrophysics |volume=643 |pages=A94 |doi=10.1051/0004-6361/202038677 |arxiv=2009.13403 |bibcode=2020A&A...643A..94L |issn=0004-6361}}</ref>
|style="text-align:center;"|←
| data-sort-value="1.99"|1.99 {{±|0.16|0.14}}<ref name=":20" />
| One of the hottest known exoplanets.
|-
|
| [[HAT-P-65|HAT-P-65b]]
| data-sort-value="1.611"|1.611 ± 0.024<ref name=":24">{{Citation |last1=Kang |first1=Huiyi |title=Simultaneous multicolour transit photometry of hot Jupiters HAT-P-19b, HAT-P-51b, HAT-P-55b, and HAT-P-65b |date=2024-05-29 |arxiv=2401.03715 |last2=Chen |first2=Guo |last3=Palle |first3=Enric |last4=Murgas |first4=Felipe |last5=Garcia |first5=Nestor Abreu |last6=Leon |first6=Jerome de |last7=Enoc |first7=Gareb |last8=Esparza-Borges |first8=Emma |last9=Fukuda |first9=Izuru|journal=Monthly Notices of the Royal Astronomical Society |volume=528 |issue=2 |pages=1930–1944 |doi=10.1093/mnras/stae072 |doi-access=free}}</ref>
|style="text-align:center;"|←
| data-sort-value="0.554"|0.554 {{±|0.092|0.091}}<ref name=":24" />
|
|-
|
| [[NGTS-31 b]]
| data-sort-value="1.61"|1.61 ± 0.16<ref name="NGTS-31 and 32">{{Cite journal |last1=Vines |first1=Jose I |last2=Jenkins |first2=James S |last3=Anderson |first3=David R |last4=Alves |first4=Douglas R |last5=Moyano |first5=Maximiliano |last6=Acton |first6=Jack S |last7=Apergis |first7=Ioannis |last8=Barkaoui |first8=Khalid |last9=Bayliss |first9=Daniel |last10=Bouchy |first10=Francois |last11=Bryant |first11=Edward M |last12=Burleigh |first12=Matthew R |last13=Casewell |first13=Sarah L |last14=Christiansen |first14=Jessie L |last15=Collins |first15=Karen A |date=2024-11-28 |title=NGTS-31b and NGTS-32b: Two Inflated hot Jupiters Orbiting Subgiant Stars |journal=Monthly Notices of the Royal Astronomical Society |volume=536 |issue=3 |pages=2011–2024 |doi=10.1093/mnras/stae2616 |doi-access=free |issn=0035-8711}}</ref>
|style="text-align:center;"|←
| data-sort-value="1.12"|1.12 ± 0.12<ref name="NGTS-31 and 32"/>
| 
|-
|
| [[HATS-11b]]
| data-sort-value="1.609"|1.609 ± 0.064<ref name=HATS-11b>{{Cite journal |last1=Livingston |first1=John H. |last2=Crossfield |first2=Ian J. M. |last3=Petigura |first3=Erik A. |last4=Gonzales |first4=Erica J. |last5=Ciardi |first5=David R. |last6=Beichman |first6=Charles A. |last7=Christiansen |first7=Jessie L. |last8=Dressing |first8=Courtney D. |last9=Henning |first9=Thomas |last10=Howard |first10=Andrew W. |last11=Isaacson |first11=Howard |last12=Fulton |first12=Benjamin J. |last13=Kosiarek |first13=Molly |last14=Schlieder |first14=Joshua E. |last15=Sinukoff |first15=Evan |date=2018-12-01 |title=Sixty Validated Planets from K2 Campaigns 5-8 |journal=The Astronomical Journal |volume=156 |issue=6 |pages=277 |doi=10.3847/1538-3881/aae778 |doi-access=free |arxiv=1810.04074 |bibcode=2018AJ....156..277L |issn=0004-6256}}</ref>
|style="text-align:center;"|←
| data-sort-value="0.85"|0.85<ref name=HATS-11b />
| 
|-
|
| [[K2-52b]]
| data-sort-value="1.61"|1.61 ± 0.20<ref name=K2-52b>{{Cite journal |last1=Livingston |first1=John H. |last2=Crossfield |first2=Ian J. M. |last3=Werner |first3=Michael W. |last4=Gorjian |first4=Varoujan |last5=Petigura |first5=Erik A. |last6=Ciardi |first6=David R. |last7=Dressing |first7=Courtney D. |last8=Fulton |first8=Benjamin J. |last9=Hirano |first9=Teruyuki |last10=Schlieder |first10=Joshua E. |last11=Sinukoff |first11=Evan |last12=Kosiarek |first12=Molly |last13=Akeson |first13=Rachel |last14=Beichman |first14=Charles A. |last15=Benneke |first15=Björn |date=2019-03-01 |title=Spitzer Transit Follow-up of Planet Candidates from the K2 Mission |journal=The Astronomical Journal |volume=157 |issue=3 |pages=102 |doi=10.3847/1538-3881/aaff69 |doi-access=free |arxiv=1901.05855 |bibcode=2019AJ....157..102L |issn=0004-6256}}</ref>
|style="text-align:center;"|←
| <!-- data-sort-value=""|<insert mass><ref name=K2-52b /> -->
| 
|-
|
| [[KELT-7b]]
| data-sort-value="1.601"|1.60 ± 0.06<ref name="Stassun-2017" />
| style="text-align:center;"|←
| data-sort-value="1.39"|1.39 ± 0.22<ref name="Stassun-2017" />
|
|-style="background:#cff7c1"
| style="border:4px ridge blue; background:#000000; text-align:center;" |[[File:SR 12 + companion Hubble.jpg|112x112px]]
| [[SR 12 (star)|SR 12 c]]<br />''(SR 12 (AB) b,<br /> SR 12 C)''
| data-sort-value="1.6" |~ 1.6,<ref name=":11">{{Cite journal |last1=Wu |first1=Ya-Lin |last2=Bowler |first2=Brendan P. |last3=Sheehan |first3=Patrick D. |last4=Close |first4=Laird M. |last5=Eisner |first5=Joshua A. |last6=Best |first6=William M. J. |last7=Ward-Duong |first7=Kimberly |last8=Zhu |first8=Zhaohuan |last9=Kraus |first9=Adam L. |date=2022-05-01 |title=ALMA Discovery of a Disk around the Planetary-mass Companion SR 12 c |journal=The Astrophysical Journal Letters |volume=930 |issue=1 |pages=L3 |arxiv=2204.06013 |bibcode=2022ApJ...930L...3W |doi=10.3847/2041-8213/ac6420 |doi-access=free |issn=2041-8205}}</ref><br />2.38 {{±|0.27|0.32}}<ref name="Bryan-2020" />
| style="text-align:center;" |?
| data-sort-value="11" |11 ± 3<ref name=":11" />
| The planet is at the very edge of the [[deuterium burning]] limit. This object orbits around [[SR 12 (star)|SR 12 AB]] at the distance of 980 {{val|ul=AU}} but has a [[circumplanetary disk]], detected in [[Submillimetre astronomy|sub-mm]] with [[Atacama Large Millimeter Array|ALMA]].<ref name=":11" /><br />Other sources of masses includes 14 {{±|7|8}} {{Jupiter mass|link=y}},<ref name=":9" /> 12{{snd}}15 {{Jupiter mass|link=y}}<ref name=":10" /> and 13 ± 2 {{Jupiter mass|link=y}}.<ref name="Bryan-2020" />
|-
! colspan="6" style="background:#efefef" data-sort-value="1.699999" | A few notable examples with radii below 1.6 {{Jupiter radius}} ({{#expr: (71492 * 1.6) / 6378 round 2}} {{Earth radius|link=y}}).
|-
| style="border:4px ridge orange; background:#000000; text-align:center;"|[[File:Exoplanet Comparison Kepler-7 b.png|112x112px]]
| [[Kepler-7b]]
| data-sort-value="1.574"|1.574 {{±|0.075|0.071}}<ref name="Berger-2018" />
| style="text-align:center;" |←
| data-sort-value="0.433"|0.433 {{±|0.040|0.041}}<ref name="qGKCN" />
| One of the first five exoplanets to be confirmed by the [[Kepler space telescope|Kepler]] spacecraft, within 34 days of Kepler's science operations,<ref name="Latham2010" /> and the first exoplanet to have a crude map of cloud coverage.<ref name="NASA-20130930" /><ref name="MIT-20131002" /><ref name="ArXiv-20130930" />
|-
| style="border:4px ridge blue; background:#000000; text-align:center;"|[[File:Hubble Space Telescope image showing one possible orbit (dashed ellipse) of the 11-Jupiter-mass exoplanet HD 106906 b.png|112x112px]]
| [[HD 106906 b]]
| data-sort-value="1.54"|1.54 {{±|0.04|0.05}}<ref name=Bryan>{{Cite journal |last1=Bryan |first1=Marta L. |last2=Ginzburg |first2=Sivan |last3=Chiang |first3=Eugene |last4=Morley |first4=Caroline |last5=Bowler |first5=Brendan P. |last6=Xuan |first6=Jerry W. |last7=Knutson |first7=Heather A. |date=2020-12-01 |title=As the Worlds Turn: Constraining Spin Evolution in the Planetary-mass Regime |bibcode=2020ApJ...905...37B |journal=The Astrophysical Journal |volume=905 |issue=1 |pages=37 |doi=10.3847/1538-4357/abc0ef |doi-access=free |arxiv=2010.07315 |issn=0004-637X}}</ref>
| style="text-align:center;" |←
| data-sort-value="11"|11 ± 2<ref name="Bailey2014">{{cite journal |title=HD 106906 b: A planetary-mass companion outside a massive debris disk |journal=[[The Astrophysical Journal Letters]] |first1=Vanessa |last1=Bailey |first2=Tiffany |last2=Meshkat |first3=Megan |last3=Reiter |first4=Katie |last4=Morzinski |first5=Jared |last5=Males |first6=Kate Y. L. |last6=Su |first7=Philip M. |last7=Hinz |first8=Matthew |last8=Kenworthy |first9=Daniel |last9=Stark |first10=Eric |last10=Mamajek |first11=Runa |last11=Briguglio |first12=Laird M. |last12=Close |first13=Katherine B. |last13=Follette |first14=Alfio |last14=Puglisi |first15=Timothy |last15=Rodigas |first16=Alycia J. |last16=Weinberger |first17=Marco |last17=Xompero |display-authors=1 |volume=780 |issue=1 |page=L4 |date=January 2014 |arxiv=1312.1265 |doi=10.1088/2041-8205/780/1/L4 |bibcode=2014ApJ...780L...4B|s2cid=119113709}}</ref>
| This planet orbits around [[HD 106906]] at the distance of 738 [[Astronomical unit|AU]], a distance much larger than what is possible for a planet [[Nebular hypothesis|formed]] within a [[protoplanetary disk]].<ref name="IBT2">{{cite news |last=Osborne |first=Hannah |date=December 6, 2013 |title=Mystery Planet 'That Shouldn't Exist' Baffles Astronomers |url=http://www.ibtimes.co.uk/articles/528146/20131206/mystery-planet-exist-location-young-star-formation.htm |url-status=dead |archive-url=https://web.archive.org/web/20131213065309/http://www.ibtimes.co.uk/articles/528146/20131206/mystery-planet-exist-location-young-star-formation.htm |archive-date=December 13, 2013 |access-date=December 8, 2013 |work=[[International Business Times]]}}</ref> It more likely [[Star formation|formed on its own]], like a star, rather in a protoplanetary disk.<ref name="Adams2023">{{Cite journal |last1=Adams |first1=Arthur D. |last2=Meyer |first2=Michael R. |last3=Howe |first3=Alex R. |last4=Burningham |first4=Ben |last5=Daemgen |first5=Sebastian |last6=Fortney |first6=Jonathan |last7=Line |first7=Mike |last8=Marley |first8=Mark |last9=Quanz |first9=Sascha P. |last10=Todorov |first10=Kamen |date=2023-11-01 |title=Atmospheric Retrieval of L Dwarfs: Benchmarking Results and Characterizing the Young Planetary Mass Companion HD 106906 b in the Near-infrared |journal=The Astronomical Journal |volume=166 |issue=5 |pages=192 |arxiv=2309.10188 |bibcode=2023AJ....166..192A |doi=10.3847/1538-3881/acfb87 |issn=0004-6256 |doi-access=free}}</ref><br />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]].<ref name="Planet Nine">{{Cite web|url=http://www.nasa.gov/feature/goddard/2020/hubble-pins-down-weird-exoplanet-with-far-flung-orbit|title=Hubble Pins Down Weird Exoplanet with Far-Flung Orbit|first=Lynn|last=Jenner|date=December 9, 2020|website=NASA}}</ref><ref>{{Cite web|url=https://scitechdaily.com/hubble-discovers-a-strange-exoplanet-that-resembles-the-long-sought-planet-nine/|title=Hubble Discovers a Strange Exoplanet That Resembles the Long-Sought "Planet Nine"|date=December 11, 2020}}</ref>
|- style="background:pink;"
| style="border:4px ridge blue; background:#000000; text-align:center;"|[[File:New shot of Proxima Centauri, our nearest neighbour.jpg|112x112px]]
| [[Proxima Centauri]]<br />''(Alpha Centauri C)''
| data-sort-value="1.50"|1.50 ± 0.04<ref name="KervellaThévenin2017" /> <br />(0.1542 ± 0.0045 {{Solar radius|link=y}})
| style="text-align:center;" |{{number sign}}
| data-sort-value="127.9"|127.9 ± 2.3<ref name="KervellaThévenin2017" /><br />{{nowrap|(0.1221 ± 0.0022 {{Solar mass|link=y}})}}
| The [[List of nearest stars|nearest]] star and [[planetary system]] to the [[Sun]], at a distance of {{cvt|4.24|ly|pc|lk=on|abbr=off}}, orbiting around [[Alpha Centauri]] [[Alpha Centauri#Alpha Centauri AB System|AB System]], the [[List of nearest stars|nearest star system]] to the Sun. Age: 4.85 [[Gigayear|Gyr]].<ref name="ESO2003" /><br />Has a confirmed planet, [[Proxima Centauri b]],<ref name="1vpJT" /> a disputed planet, [[Proxima Centauri c]],<ref name="ArtigauCadieux2022">{{cite journal|last1=Artigau|first1=Étienne|last2=Cadieux|first2=Charles |last3=Cook|first3=Neil J.|last4=Doyon|first4=René|last5=Vandal|first5=Thomas|last6=Donati|first6=Jean-Françcois|last7=Moutou |first7=Claire|last8=Delfosse|first8=Xavier|last9=Fouqué|first9=Pascal|last10=Martioli|first10=Eder|last11=Bouchy|first11=François |last12=Parsons|first12=Jasmine|last13=Carmona|first13=Andres|last14=Dumusque|first14=Xavier|last15=Astudillo-Defru|first15=Nicola |last16=Bonfils|first16=Xavier|last17=Mignon|first17=Lucille|display-authors=5 |title=Line-by-line velocity measurements, an outlier-resistant method for precision velocimetry |journal=The Astronomical Journal|volume=164:84|issue=3|pages=18pp|arxiv=2207.13524 |bibcode=2022AJ....164...84A|doi=10.3847/1538-3881/ac7ce6|doi-access=free|date=June 23, 2022|publication-date=August 8, 2022}}</ref> and a unconfirmed planet, [[Proxima Centauri d]].<br /><small>''Reported for reference.''</small>
|-
| style="border:4px ridge green; background:#000000; text-align:center;"|[[File:Beta Pictoris.jpg|112x112px]]
| [[Beta Pictoris b]]<br />''(β Pic b)''
| data-sort-value="1.46"|1.46 ± 0.01<ref name="vbdKI" />
| style="text-align:center;" |←
| data-sort-value="11.729"|11.729 {{±|2.337|2.135}}<ref name="o5PbX" />
| First exoplanet to have its rotation rate measured and fastest-spinning exoplanet known at the time of discovery.<ref name=eso>{{cite news |url=http://www.eso.org/public/news/eso1414/ |title=Length of Exoplanet Day Measured for First Time / VLT measures the spin of Beta Pictoris b |date=April 30, 2014}}</ref><ref name="Cowen2014">{{Cite journal | doi = 10.1038/nature.2014.15132| title = First exoplanet seen spinning| journal = Nature| date = April 30, 2014| last1 = Cowen | first1 = R. | s2cid = 123849861}}</ref> Beta Pictoris b is suspected to have [[Beta Pictoris b#Potential exomoon|exomoon]] due to the former's predicted [[obliquity]] misalignment.<ref name=Michael2024>{{Cite journal |last1=Poon |first1=Michael |last2=Rein |first2=Hanno |last3=Pham |first3=Dang |title=A potential exomoon from the predicted planet obliquity of <a:math xmlns:a="http://www.w3.org/1998/Math/MathML"> <a:mi>β</a:mi> </a:math> Pictoris b |journal=The Open Journal of Astrophysics |date=2024-12-08 |volume=7 |doi=10.33232/001c.127130 |arxiv=2412.05988}}</ref>
|-
| style="border:4px ridge blue; background:#000000; text-align:center;"|[[File:The unusual exoplanet HIP 65426b — SPHERE's first.jpg|112px]]
| [[Najsakopajk]]<br />''(HIP 65426 b)''
| data-sort-value="1.44"|1.44 ± 0.03<ref name="Carter et al">{{cite journal |last1=Carter |first1=Aarynn L. |last2=Hinkley |first2=Sasha |last3=Kammerer |first3=Jens |last4=Skemer |first4=Andrew |last5=Biller |first5=Beth A. |last6=Leisenring |first6=Jarron M. |last7=Millar-Blanchaer |first7=Maxwell A. |last8=Petrus |first8=Simon |last9=Stone |first9=Jordan M. |last10=Ward-Duong |first10=Kimberly |last11=Wang |first11=Jason J. |last12=Girard |first12=Julien H. |last13=Hines |first13=Dean C. |last14=Perrin |first14=Marshall D. |last15=Pueyo |first15=Laurent |title=The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems I: High Contrast Imaging of the Exoplanet HIP 65426 b from 2-16 μm |arxiv=2208.14990 | doi=10.3847/2041-8213/acd93e | journal=The Astrophysical Journal Letters | date=2023-07-06 | volume=951 | issue=1 | pages=L20 |doi-access=free | bibcode=2023ApJ...951L..20C}}</ref>
| style="text-align:center;" |←
| data-sort-value="7.1"|7.1 ± 1.2, 9.9 {{±|1.1|1.8}},<br />10.9 {{±|1.4|2.0}}<ref name="Carter et al" />
| First exoplanet to be imaged by the [[James Webb Space Telescope]].<ref>Alise Fisher, NASA’s Webb Takes Its First-Ever Direct Image of Distant World Posted on September 1, [https://blogs.nasa.gov/webb/2022/09/01/nasas-webb-takes-its-first-ever-direct-image-of-distant-world/ blogs.nasa.gov]</ref> The JWST direct imaging observations tightly constrained its [[Luminosity|bolometric luminosity]], which provides a robust mass constraint of 7.1 ± 1.2 {{Jupiter mass|link=y}}. 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,<ref name="scinews">{{Cite web|url=http://www.sci-news.com/astronomy/super-jupiter-hip-65426-05023.html|title=Astronomers Directly Image Super-Jupiter around HIP 65426 {{!}} Astronomy {{!}} Sci-News.com|website=Breaking Science News {{!}} Sci-News.com|language=en-US|access-date=2019-08-02}}</ref><ref name="nasa-HIP">{{Cite web|url=https://exoplanets.nasa.gov/news/1477/holiday-special-eight-nights-of-exoplanet-light/|title=Holiday Special: Eight nights of Exoplanet Light|publisher=NASA|website=Exoplanet Exploration: Planets Beyond our Solar System|date=14 December 2017 |access-date=2019-08-03}}</ref> causing it to not fit [[Planet formation|current models for planetary formation]].<ref>{{Cite web|url=https://phys.org/news/2017-07-discovery-exoplanet-spherevlt.html|title=Odd planetary system around fast-spinning star doesn't quite fit existing models of planet formation|website=phys.org|language=en-us|access-date=2019-08-03}}</ref>
|-
| style="border:4px ridge red; background:black; text-align:center;"|[[File:Oxygen and carbon discovered in extrasolar planet atmosphere blow-off.jpg|112x112px]]
| [[HD 209458 b]]<br />''("Osiris")''
| data-sort-value="1.359"|1.359 {{±|0.016|0.019}}<ref name="Bonomo-2017a" />
| style="text-align:center;" |←
| data-sort-value="0.682"|0.682 {{±|0.014|0.015}}<ref name="Bonomo-2017a" />
| Represents multiple milestones in exoplanetary discovery, such as the first exoplanet known observed to [[Planetary transit|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 [[Spectroscopy|spectroscopically]]<ref name="Spectroscopy">{{Cite web |title=NASA's Spitzer First To Crack Open Light of Faraway Worlds |url=http://www.spitzer.caltech.edu/Media/releases/ssc2007-04/release.shtml |archive-url=https://web.archive.org/web/20070715071155/http://www.spitzer.caltech.edu/Media/releases/ssc2007-04/release.shtml |archive-date=July 15, 2007}}</ref><ref name="Richardson2007">{{cite journal |last1=Richardson |first1=L. Jeremy |last2=Deming |first2=D |last3=Horning |first3=K |last4=Seager |first4=S |last5=Harrington |first5=J |display-authors=etal |date=2007 |title=A spectrum of an extrasolar planet |journal=Nature |volume=445 |issue=7130 |pages=892–895 |arxiv=astro-ph/0702507 |bibcode=2007Natur.445..892R |doi=10.1038/nature05636 |pmid=17314975 |s2cid=4415500}}</ref> 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]]"''.
|- style="background:pink;"
| style="border:4px ridge green; background:#000000; text-align:center;"|[[File:Pleiades and Teide 1.png|116px]]
| [[Teide 1]] 
| data-sort-value="1.311"|1.311 {{±|0.120|0.075}}<ref name=":18">{{Cite journal |last1=Hurt |first1=Spencer A. |last2=Liu |first2=Michael C. |last3=Zhang |first3=Zhoujian |last4=Phillips |first4=Mark |last5=Allers |first5=Katelyn N. |last6=Deacon |first6=Niall R. |last7=Aller |first7=Kimberly M. |last8=Best |first8=William M. J. |date=2024-01-01 |title=Uniform Forward-modeling Analysis of Ultracool Dwarfs. III. Late-M and L Dwarfs in Young Moving Groups, the Pleiades, and the Hyades |journal=The Astrophysical Journal |volume=961 |issue=1 |pages=121 |arxiv=2311.04268 |bibcode=2024ApJ...961..121H |doi=10.3847/1538-4357/ad0b12 |doi-access=free |issn=0004-637X}}</ref><br />(0.1347 {{±|0.0123|0.0077}} {{Solar radius|link=y}})
| style="text-align:center;" |{{number sign}}
| data-sort-value="52"|52 {{±|15|10}}<ref name=":18" /><br />(0.0496 {{±|0.0143|0.0095}} {{val|ul=Solar mass}})
| The first [[brown dwarf]] to be confirmed.<ref name="RafaelRebolo2014" /><ref>{{Cite journal |last1=Rebolo |first1=R. |last2=Osorio |first2=M. R. Zapatero |last3=Martín |first3=E. L. |date=1995-09-14 |title=Discovery of a brown dwarf in the Pleiades star cluster |url=https://www.nature.com/articles/377129a0 |journal=Nature |language=en |volume=377 |issue=6545 |pages=129–131 |bibcode=1995Natur.377..129R |doi=10.1038/377129a0 |issn=0028-0836}}</ref> It is located in the [[Pleiades]] and has an age of 70{{snd}}140[[Million years ago|Myr]].<ref>{{Cite journal |last1=Rebolo |first1=R. |last2=Martín |first2=E. L. |last3=Basri |first3=G. |last4=Marcy |first4=G. W. |last5=Zapatero-Osorio |first5=M. R. |date=1996-09-20 |title=Brown Dwarfs in the Pleiades Cluster Confirmed by the Lithium Test |url=https://iopscience.iop.org/article/10.1086/310263 |journal=The Astrophysical Journal |volume=469 |issue=1 |pages=L53–L56 |arxiv=astro-ph/9607002 |bibcode=1996ApJ...469L..53R |doi=10.1086/310263}}</ref><br /><small>''Reported for reference.''</small>
|-
| style="border:4px ridge purple; background:white; text-align:center;"|[[File:OGLE-TR-56 b rv.pdf|112x112px]]
| [[OGLE-TR-56b]]
| data-sort-value="1.30"|1.30 ± 0.05
| style="text-align:center;" |←
| data-sort-value="1.29"|1.29 ± 0.12
| First discovered exoplanet using the [[transit method]].<ref>{{cite journal |author=[[Harvard University]] and [[Smithsonian Institution]] |date=2003-01-08 |title=New World of Iron Rain |url=http://www.astrobio.net/pressrelease/352/new-world-of-iron-rain |url-status=usurped |journal=Astrobiology Magazine |archive-url=https://web.archive.org/web/20100110135215/http://www.astrobio.net/pressrelease/352/new-world-of-iron-rain |archive-date=2010-01-10 |access-date=2010-01-25}}</ref>
|-
| style="border:4px ridge blue; background:#370A00; text-align:center;"|[[File:TOI-157.jpg|112x112px]]
| [[TOI-157b]]
| data-sort-value="1.29"|1.29 ± 0.02<ref name="oldest">{{Cite journal |last1=Nielsen |first1=L. D. |last2=Brahm |first2=R. |last3=Bouchy |first3=F. |last4=Espinoza |first4=N. |last5=Turner |first5=O. |last6=Rappaport |first6=S. |last7=Pearce |first7=L. |last8=Ricker |first8=G. |last9=Vanderspek |first9=R. |last10=Latham |first10=D. W. |last11=Seager |first11=S. |last12=Winn |first12=J. N. |last13=Jenkins |first13=J. M. |last14=Acton |first14=J. S. |last15=Bakos |first15=G. |date=July 2020 |title=Three short-period Jupiters from TESS: HIP 65Ab, TOI-157b, and TOI-169b |url=https://www.aanda.org/10.1051/0004-6361/202037941 |journal=Astronomy & Astrophysics |volume=639 |pages=A76 |arxiv=2003.05932 |bibcode=2020A&A...639A..76N |doi=10.1051/0004-6361/202037941 |issn=0004-6361}}</ref>
| style="text-align:center;" |←
| data-sort-value="1.18"|1.18 ± 0.13<ref name="oldest" />
| [[List of exoplanet extremes#Planetary characteristics|Oldest]] confirmed planet at the age of 12.9 {{±|1.4|0.69}} [[Gigayear|Gyr]]<ref name="oldest" />
|-
| style="border:4px ridge red; background:#846000; text-align:center;"|[[File:TrES-2b.png|112x112px]]
| [[TrES-2b|TrES-2]] <br />''(Kepler-1 Ab)''
| data-sort-value="1.265"|1.265 {{±|0.054|0.051}}<ref name="Berger-2018" />
| style="text-align:center;" |←
| data-sort-value="1.199"|1.199 ± 0.052<ref name="Vk5eJ" />
| Darkest known exoplanet due to an extremely low [[geometric albedo]] of 0.0136, absorbing 99% of light.
|-
|style="border:4px ridge red; background:#000000; text-align:center;"|[[File:Profile of planet 51 Pegasi b (planet only).jpg|112x112px]]
| [[Dimidium]] <br />''(51 Pegasi b)''
| data-sort-value="1.2"|1.2 ± 0.1<ref name="spring">{{Cite journal|arxiv=2201.03600 |doi=10.1051/0004-6361/202142314 |title=Black Mirror: The impact of rotational broadening on the search for reflected light from 51 Pegasi b with high resolution spectroscopy |date=2022 |last1=Spring |first1=E. F. |last2=Birkby |first2=J. L. |last3=Pino |first3=L. |last4=Alonso |first4=R. |last5=Hoyer |first5=S. |last6=Young |first6=M. E. |last7=Coelho |first7=P. R. T. |last8=Nespral |first8=D. |last9=López-Morales |first9=M. |journal=Astronomy & Astrophysics |volume=659 |pages=A121 |bibcode=2022A&A...659A.121S |s2cid=245853836}}</ref>
| style="text-align:center;" |←
| data-sort-value="0.46"|0.46 {{±|0.06|0.01}}<ref name="Martins-2015" />
| First exoplanet to be discovered orbiting a [[Main sequence|main-sequence]] star.<ref name="Peg">{{cite web |url=https://physicsworld.com/a/first-visible-light-detected-directly-from-an-exoplanet/ |title=First visible light detected directly from an exoplanet |date=2015-04-22 |work=Physicworld}}</ref> Prototype of the [[hot Jupiter]]s.
<!--
|-
| style="border:4px ridge red; background:#000000; text-align:center; "|[[File:Artist's_concept_of_Gliese_876_b.jpg|112x112px]]
| [[Gliese 876b]]
| data-sort-value="1.1925"|1.1925<ref>https://science.nasa.gov/exoplanet-catalog/gj-876-b/</ref>
| style="text-align:center;" |←
| data-sort-value="2.2756 "|2.2756,<ref name="Rivera2010" /><br />2.659 {{±|0.0299|0.0295}}<ref name="Rivera2010">{{cite journal | title=The Lick-Carnegie Exoplanet Survey: A Uranus-mass Fourth Planet for GJ 876 in an Extrasolar Laplace Configuration | last1=Rivera | first1=Eugenio J. | last2=Laughlin | first2=Gregory | last3=Butler | first3=R. Paul | last4=Vogt | first4=Steven S. | last5=Haghighipour | first5=Nader | last6=Meschiari | first6=Stefano | display-authors=1 | journal=The Astrophysical Journal | volume=719 | issue=1 | pages=890–899 |date=July 2010 | arxiv=1006.4244 | bibcode=2010ApJ...719..890R | bibcode-access=free | doi=10.1088/0004-637X/719/1/890 | doi-access=free}}</ref>{{efn|Uncertainties in the planetary masses and semimajor axes do not take into account the uncertainty in the mass of the star.}}<br />(845.2 {{±|9.5|9.4}} {{val|ul=Earth mass}})
| First planet to be discovered orbiting a [[red dwarf]]; first extrasolar [[planetary system]] around a [[normal star]] with measured [[coplanarity]] and only known system of orbital companions to exhibit a near-triple conjunction in the rare phenomenon of [[Laplace resonance]].
--> 
|-
| style="border:4px ridge green; background:#000053; text-align:center;" |[[File:HR 8799 Orbiting Exoplanets.gif|112x112px]]
| [[HR 8799 e]]
| data-sort-value="1.17" |1.17 {{±|0.13|0.11}}<ref>{{Cite journal |last1=Lacour |first1=S. |last2=Nowak |first2=M. |last3=Wang |first3=J. |last4=Pfuhl |first4=O. |last5=Eisenhauer |first5=F. |last6=Abuter |first6=R. |last7=Amorim |first7=A. |last8=Anugu |first8=N. |last9=Benisty |first9=M. |last10=Berger |first10=J. P. |last11=Beust |first11=H. |last12=Blind |first12=N. |last13=Bonnefoy |first13=M. |last14=Bonnet |first14=H. |last15=Bourget |first15=P. |date=March 2019 |title=First direct detection of an exoplanet by optical interferometry; Astrometry and K-band spectroscopy of HR8799 e |journal=Astronomy & Astrophysics |volume=623 |pages=L11 |doi=10.1051/0004-6361/201935253 |arxiv=1903.11903 |bibcode=2019A&A...623L..11G |s2cid=85542913 |issn=0004-6361}}</ref>
| style="text-align:center;" |←
| data-sort-value="9.6" |9.6 {{±|1.9|1.8}}<ref>{{Cite journal |last1=Brandt |first1=G. Mirek |last2=Brandt |first2=Timothy D. |last3=Dupuy |first3=Trent J. |last4=Michalik |first4=Daniel |last5=Marleau |first5=Gabriel-Dominique |date=2021-07-01 |title=The First Dynamical Mass Measurement in the HR 8799 System |journal=The Astrophysical Journal Letters |volume=915 |issue=1 |pages=L16 |arxiv=2105.12820 |bibcode=2021ApJ...915L..16B |doi=10.3847/2041-8213/ac0540 |doi-access=free |issn=2041-8205}}</ref>
| First exoplanet to be directly observed using [[optical interferometry]]. [[HR 8799]] system is also the first [[direct imaging|directly imaged]] [[planetary system]] having multiple [[exoplanet]]s.
|- style="background:pink;"
| style="border:4px ridge red; background:black; text-align:center;" |[[File:Artist's view of planets transiting red dwarf star in TRAPPIST-1 system.jpg|112x112px]]
| [[TRAPPIST-1]]
| data-sort-value="1.16" |1.16 ± 0.01<ref name=":25">{{Cite journal |last1=Agol |first1=Eric |last2=Dorn |first2=Caroline |last3=Grimm |first3=Simon L. |last4=Turbet |first4=Martin |last5=Ducrot |first5=Elsa |last6=Delrez |first6=Laetitia |last7=Gillon |first7=Michaël |last8=Demory |first8=Brice-Olivier |last9=Burdanov |first9=Artem |last10=Barkaoui |first10=Khalid |last11=Benkhaldoun |first11=Zouhair |last12=Bolmont |first12=Emeline |last13=Burgasser |first13=Adam |last14=Carey |first14=Sean |last15=de Wit |first15=Julien |date=2021-02-01 |title=Refining the Transit-timing and Photometric Analysis of TRAPPIST-1: Masses, Radii, Densities, Dynamics, and Ephemerides |journal=The Planetary Science Journal |volume=2 |issue=1 |pages=1 |arxiv=2010.01074 |bibcode=2021PSJ.....2....1A |doi=10.3847/PSJ/abd022 |doi-access=free |issn=2632-3338}}</ref><br /> (0.1192 ± 0.0013 {{Solar radius|link=y}})
| style="text-align:center;" |{{number sign}}
| data-sort-value="94.1" |94.1 ± 2.4<ref name=":25" /><br />{{nowrap|(0.0898 ± 0.0023 {{Solar mass|link=y}})}}
| [[List of exoplanet extremes|Coldest and smallest]] known star hosting exoplanets.<ref>{{Cite journal |last1=Delrez |first1=L. |last2=Murray |first2=C. A. |last3=Pozuelos |first3=F. J. |last4=Narita |first4=N. |last5=Ducrot |first5=E. |last6=Timmermans |first6=M. |last7=Watanabe |first7=N. |last8=Burgasser |first8=A. J. |last9=Hirano |first9=T. |last10=Rackham |first10=B. V. |last11=Stassun |first11=K. G. |last12=Van Grootel |first12=V. |last13=Aganze |first13=C. |last14=Cointepas |first14=M. |last15=Howell |first15=S. |date=November 2022 |title=Two temperate super-Earths transiting a nearby late-type M dwarf |url=https://www.aanda.org/10.1051/0004-6361/202244041 |journal=Astronomy & Astrophysics |volume=667 |pages=A59 |arxiv=2209.02831 |bibcode=2022A&A...667A..59D |doi=10.1051/0004-6361/202244041 |issn=0004-6361}}</ref> All [[TRAPPIST-1#Planetary system|seven exoplanets]] are rocky planets, orbiting closer to the star than [[Mercury (planet)#Orbit, rotation, and longitude|Mercury]]. Their orbits' inclinations of 0.1 degrees{{sfn|Agol|Dorn|Grimm|Turbet|2021|p=14}} makes TRAPPIST-1 system the flattest [[planetary system]].<ref>{{cite journal |last1=Heising |first1=Matthew Z. |last2=Sasselov |first2=Dimitar D. |last3=Hernquist |first3=Lars |last4=Luisa Tió Humphrey |first4=Ana |title=How Flat Can a Planetary System Get? I. The Case of TRAPPIST-1 |journal=The Astrophysical Journal |date=1 June 2021 |volume=913 |issue=2 |bibcode=2021ApJ...913..126H |doi=10.3847/1538-4357/abf8a8 |s2cid=219262616 |language=en|doi-access=free|page=126}}</ref> Age: 7.6 ± 2.2 [[Gigayear|Gyr]].<ref>{{Cite journal |last1=Burgasser |first1=Adam J. |last2=Mamajek |first2=Eric E. |date=2017-08-20 |title=On the Age of the TRAPPIST-1 System |journal=The Astrophysical Journal |volume=845 |issue=2 |pages=110 |arxiv=1706.02018 |bibcode=2017ApJ...845..110B |doi=10.3847/1538-4357/aa7fea |doi-access=free |issn=0004-637X}}</ref><br /><small>''Reported for reference.''</small>
|-
| style="border:4px ridge red; background:#000000; text-align:center;" |[[File:Artist’s impression of the deep blue planet HD 189733b.jpg|112x112px]]
| [[HD 189733 Ab]] 
| data-sort-value="1.138" |1.138 ± 0.027<ref name="Bonomo-2017a">{{Cite journal |last1=Bonomo |first1=A. S. |last2=Desidera |first2=S. |last3=Benatti |first3=S. |last4=Borsa |first4=F. |last5=Crespi |first5=S. |last6=Damasso |first6=M. |last7=Lanza |first7=A. F. |last8=Sozzetti |first8=A. |last9=Lodato |first9=G. |last10=Marzari |first10=F. |last11=Boccato |first11=C. |last12=Claudi |first12=R. U. |last13=Cosentino |first13=R. |last14=Covino |first14=E. |last15=Gratton |first15=R. |date=June 2017 |title=The GAPS Programme with HARPS-N at TNG: XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets⋆ |url=http://www.aanda.org/10.1051/0004-6361/201629882 |journal=Astronomy & Astrophysics |volume=602 |pages=A107 |arxiv=1704.00373 |bibcode=2017A&A...602A.107B |doi=10.1051/0004-6361/201629882 |issn=0004-6361}}</ref>
| style="text-align:center;" |←
| data-sort-value="1.123" |1.123 ± 0.045<ref name="Bonomo-2017a" />
| First exoplanet to have its [[heat map|thermal map]] constructed,<ref name="Knutson2007" /> its overall color (deep blue) determined,<ref name="Berdyugina2011" /><ref name="Evans2013" /> its transit viewed in the X-ray spectrum, one of first two exoplanets (other being [[HD 209458 b|"Osiris"]]) to be observed [[Spectroscopy|spectroscopically]]<ref name="Spectroscopy">{{Cite web |title=NASA's Spitzer First To Crack Open Light of Faraway Worlds |url=http://www.spitzer.caltech.edu/Media/releases/ssc2007-04/release.shtml |archive-url=https://web.archive.org/web/20070715071155/http://www.spitzer.caltech.edu/Media/releases/ssc2007-04/release.shtml |archive-date=July 15, 2007}}</ref><ref name="Richardson2007">{{cite journal |last1=Richardson |first1=L. Jeremy |last2=Deming |first2=D |last3=Horning |first3=K |last4=Seager |first4=S |last5=Harrington |first5=J |display-authors=etal |date=2007 |title=A spectrum of an extrasolar planet |journal=Nature |volume=445 |issue=7130 |pages=892–895 |arxiv=astro-ph/0702507 |bibcode=2007Natur.445..892R |doi=10.1038/nature05636 |pmid=17314975 |s2cid=4415500}}</ref> and first to have [[carbon dioxide]] confirmed as being present in its atmosphere.<br />Such the rich [[cobalt blue]]<ref name="jz7Ys" /><ref name="qWEUO" /> colour of HD 189733 Ab may be the result of [[Rayleigh scattering]]. The wind can blow up to {{convert|8700|km/h|mph|abbr=on}} from the day side to the night side.<ref name="h1pFg" />
|- style="background:#FFE8DC"
| style="border:4px ridge blue; background:#000000; text-align:center;" |[[File:2M1207b - First image of an exoplanet.jpg|112px]]
| [[2M1207 b]]<br />''(TWA 27b)''
| data-sort-value="1.13"|1.13<ref name="Luhman" />
| style="text-align:center;" |{{dagger}}
| data-sort-value="5.5"|5.5 ± 0.5<ref name="Luhman" />
| First [[Planetary-mass object|planetary body]] discovered via direct imaging, and the first around a [[brown dwarf]].<ref>{{Cite web |title=2M1207 b - First image of an exoplanet - NASA Science |url=https://science.nasa.gov/resource/2m1207-b-first-image-of-an-exoplanet/ |access-date=2025-01-07 |website=science.nasa.gov |date=26 April 2010 |language=en-US}}</ref><ref>{{Cite web |last= |title=2M1207b - first image of an exoplanet |url=https://www.eso.org/public/unitedkingdom/images/26a_big-vlt/?lang |access-date=2025-01-07 |website=[[European Southern Observatory]] |language=en-gb}}</ref> 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 {{Jupiter mass|26|link=y}} brown dwarf, a ratio much larger than the 1:1000 of Jupiter and Sun for example. The [[International Astronomical Union|IAU]] defined that exoplanets must have a mass ratio to the central object less than 0.04,<ref name="IAU-definition2">{{cite web |title=Official Working Definition of an Exoplanet |url=https://www.iau.org/science/scientific_bodies/commissions/F2/info/documents/ |access-date=29 November 2020 |work=IAU position statement}}</ref><ref name="LecavelierEtangs20222">{{Cite journal |last1=Lecavelier des Etangs |first1=A. |last2=Lissauer |first2=Jack J. |date=June 2022 |title=The IAU working definition of an exoplanet |url=https://linkinghub.elsevier.com/retrieve/pii/S138764732200001X |journal=New Astronomy Reviews |language=en |volume=94 |pages=101641 |arxiv=2203.09520 |bibcode=2022NewAR..9401641L |doi=10.1016/j.newar.2022.101641 |s2cid=247065421}}</ref> which would make 2M1207b a sub-brown dwarf. Nevertheless, 2M1207b has been considered an exoplanet by press media and websites,<ref name="Spacecom-2005">{{Cite web |last=Britt |first=Robert Roy |date=April 30, 2005 |title=Fresh Debate over First Photo of Extrasolar Planet |url=https://www.space.com/1023-fresh-debate-photo-extrasolar-planet.html |access-date=June 16, 2008 |website=Space.com}}</ref><ref>{{Cite web |title=The brown dwarf 2M1207 and its planetary companion |url=https://www.eso.org/public/unitedkingdom/images/eso0515a/?lang |access-date=2025-01-07 |website=[[European Southern Observatory]] |language=en-gb}}</ref><ref>{{Cite web |title=Artist's View of a Super-Jupiter around a Brown Dwarf (2M1207) |url=https://esahubble.org/images/opo1605a/ |access-date=2025-01-07 |website=Esa Hubble |language=en}}</ref> exoplanet databases<ref>{{Cite Exoplanet Archive|2MASS J12073346-3932539}}</ref><ref>{{Cite EPE|name=2M1207 b|id=237}}</ref> and alternative definitions.<ref>{{Citation |last1=Margot |first1=Jean-Luc |title=Quantitative Criteria for Defining Planets |date=2024-07-10 |arxiv=2407.07590 |last2=Gladman |first2=Brett |last3=Yang |first3=Tony|journal=The Planetary Science Journal |volume=5 |issue=7 |page=159 |doi=10.3847/PSJ/ad55f3 |doi-access=free |bibcode=2024PSJ.....5..159M}}</ref> It will shrink to a size slightly smaller than [[Jupiter radius|Jupiter]] as it cools over the next few billion years.
|- style="background:pink;"
| 
| [[2MASS J0523−1403]]
| data-sort-value="1.126"|1.126 ± 0.063<ref name=":26">{{Cite journal |last1=Cifuentes |first1=C. |last2=Caballero |first2=J. A. |last3=Cortés-Contreras |first3=M. |last4=Montes |first4=D. |last5=Abellán |first5=F. J. |last6=Dorda |first6=R. |last7=Holgado |first7=G. |last8=Zapatero Osorio |first8=M. R. |last9=Morales |first9=J. C. |last10=Amado |first10=P. J. |last11=Passegger |first11=V. M. |last12=Quirrenbach |first12=A. |last13=Reiners |first13=A. |last14=Ribas |first14=I. |last15=Sanz-Forcada |first15=J. |date=October 2020 |title=CARMENES input catalogue of M dwarfs: V. Luminosities, colours, and spectral energy distributions |url=https://www.aanda.org/10.1051/0004-6361/202038295 |journal=Astronomy & Astrophysics |volume=642 |pages=A115 |arxiv=2007.15077 |bibcode=2020A&A...642A.115C |doi=10.1051/0004-6361/202038295 |issn=0004-6361}}</ref><br />(0.116 ± 0.006 {{Solar radius|link=y}})
| style="text-align:center;" |{{number sign}}
| data-sort-value="103"|103 ± 11<ref name=":26" /><br />(0.0983 ± 0.0011 {{Solar mass|link=y}})<br />or<br />67.54 ± 12.79<ref name="filippazzo">{{cite journal |last1=Filippazzo |first1=Joseph C. |last2=Rice |first2=Emily L. |last3=Faherty |first3=Jacqueline |author3-link=Jackie Faherty |last4=Cruz |first4=Kelle L. |last5=Van Gordon |first5=Mollie M. |last6=Looper |first6=Dagny L. |year=2015 |title=Fundamental Parameters and Spectral Energy Distributions of Young and Field Age Objects with Masses Spanning the Stellar to Planetary Regime |journal=The Astrophysical Journal |volume=810 |issue=2 |pages=158 |arxiv=1508.01767 |bibcode=2015ApJ...810..158F |doi=10.1088/0004-637X/810/2/158 |s2cid=89611607}}</ref><br />(0.0644 ± 0.0122 {{Solar mass|link=y}})
| [[List of coolest stars|Coolest]] [[main sequence]] star with [[effective temperature]] 1939 [[Kelvin|K]] (1666 {{val|ul=°C}}; 3031 {{val|ul=°F}})<ref name="filippazzo" /> and [[List of smallest known stars|one of the smallest stars]], in both radius and mass.<ref name=Dieterich_2013>{{cite journal | last1 = Dieterich | first1 = Sergio B. | last2 = Henry | first2 = Todd J. | last3 = Jao | first3 = Wei-Chun | last4 = Winters | first4 = Jennifer G. | last5 = Hosey | first5 = Altonio D. | last6 = Riedel | first6 = Adric R. | last7 = Subasavage | first7 = John P. | title = The Solar Neighborhood XXXII. The Hydrogen Burning Limit | journal = [[The Astronomical Journal]] | volume = 147 | issue = 5 | at = article id 94 | date = May 2014 | doi = 10.1088/0004-6256/147/5/94 | bibcode = 2014AJ....147...94D | arxiv = 1312.1736 | s2cid = 21036959}}</ref><br /><small>''Reported for reference.''</small>
|- 
|style="border:4px ridge blue; background:#000000; text-align:center;"| [[File:GJ900 AB unWISE.jpg|112x112px]]
| [[Gliese 900 b]]<br />''(CW2335+0142)''
| data-sort-value="1.11"|1.11<ref>{{Cite web |title=GJ 900 b - NASA Science |url=https://science.nasa.gov/exoplanet-catalog/gj-900-b/ |access-date=2024-06-20 |website=science.nasa.gov |date=31 May 2024 |language=en-US}}</ref>
| style="text-align:center;" |←
| data-sort-value="10.5"|10.5<ref>{{Cite journal |last1=Rothermich |first1=Austin |last2=Faherty |first2=Jacqueline K. |last3=Bardalez-Gagliuffi |first3=Daniella |last4=Schneider |first4=Adam C. |last5=Kirkpatrick |first5=J. Davy |last6=Meisner |first6=Aaron M. |last7=Burgasser |first7=Adam J. |last8=Kuchner |first8=Marc |last9=Allers |first9=Katelyn |last10=Gagné |first10=Jonathan |last11=Caselden |first11=Dan |last12=Calamari |first12=Emily |last13=Popinchalk |first13=Mark |last14=Suárez |first14=Genaro |last15=Gerasimov |first15=Roman |date=2024-06-01 |title=89 New Ultracool Dwarf Comoving Companions Identified with the Backyard Worlds: Planet 9 Citizen Science Project |journal=The Astronomical Journal |volume=167 |issue=6 |pages=253 |arxiv=2403.04592 |bibcode=2024AJ....167..253R |doi=10.3847/1538-3881/ad324e |issn=0004-6256 |doi-access=free}}</ref>
| This exoplanet has the largest observed host star separation of any known exoplanet, at 12 000 [[Astronomical unit|AU]] (0.058 [[Parsec|pc]]; 0.19 [[Light-year|ly]]) and the longest known orbital period, at a duration of 1.27 [[Year#SI prefix multipliers|Myr]]. First confirmed and third discovered [[circumtriple planet]].
|- style="background:#FFF8DC"
| style="border:4px ridge yellow; background:#000000; text-align:center;" |[[File:Exoplanet Comparison CoRoT-3 b.png|112px]]
| [[CoRoT-3b|CoRoT-3 Ab]]
| data-sort-value="1.085"|1.08 ± 0.05<ref name="8YMrE" />
| style="text-align:center;" |{{asterisk}}
| data-sort-value="21.66"|21.66 ± 1.00<ref name="Deleuil2008" />
| Might be considered either a [[exoplanet|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 fusion|deuterium burning]] limit as the delimiter (i.e. {{val|13|u=Jupiter mass}}), CoRoT-3b is a brown dwarf.<ref name="3YVJQ" /> 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 [[accretion (astrophysics)|core accretion]].<ref name="fny8Y" /> However, it is unclear which method of formation created CoRoT-3A b.
|-
| style="border:4px ridge red; background:#000000; text-align:center;" |[[File:KEPLER 1647 (AB) b.png|112px]]
| [[Kepler-1647 b]]
| data-sort-value="1.05932"|1.05932 ± 0.01228<ref name="NASA-Exoplanet-Archive - Kepler-1647b">{{cite web |url=http://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=Kepler-1647+b&type=CONFIRMED_PLANET |title=Kepler-1647b – NASA Exoplanet Archive | access-date=June 14, 2016}}</ref>
| style="text-align:center;" |←
| data-sort-value="1.52"|1.52 ± 0.65<ref name="NASA-Exoplanet-Archive - Kepler-1647b" />
| Longest transit orbital period of any confirmed transiting exoplanet discovered at the duration of 1107 days<ref name="NASA-Goddard">{{cite web |url=https://www.nasa.gov/feature/goddard/2016/new-planet-is-largest-discovered-that-orbits-two-suns |title=New Planet Is Largest Discovered That Orbits Two Suns |publisher=[[NASA]] |date=June 13, 2016 |access-date=June 14, 2016}}</ref> and largest [[circumbinary planet]] discovered.<ref name="arxiv">{{cite journal |title=Kepler-1647b: the largest and longest-period Kepler transiting circumbinary planet |arxiv=1512.00189 |last1=Kostov |first1=Veselin B. |last2=Orosz |first2=Jerome A. |last3=Welsh |first3=William F. |last4=Doyle |first4=Laurance R. |last5=Fabrycky |first5=Daniel C. |last6=Haghighipour |first6=Nader |last7=Quarles |first7=Billy |last8=Short |first8=Donald R. |last9=Cochran |first9=William D. |last10=Endl |first10=Michael |last11=Ford |first11=Eric B. |last12=Gregorio |first12=Joao |last13=Hinse |first13=Tobias C. |last14=Isaacson |first14=Howard |last15=Jenkins |first15=Jon M. |last16=Jensen |first16=Eric L. N. |last17=Kane |first17=Stephen |last18=Kull |first18=Ilya |last19=Latham |first19=David W. |last20=Lissauer |first20=Jack J. |last21=Marcy |first21=Geoffrey W. |last22=Mazeh |first22=Tsevi |last23=Muller |first23=Tobias W. A. |last24=Pepper |first24=Joshua |last25=Quinn |first25=Samuel N. |last26=Ragozzine |first26=Darin |last27=Shporer |first27=Avi |last28=Steffen |first28=Jason H. |last29=Torres |first29=Guillermo |last30=Windmiller |first30=Gur |display-authors=15 |year=2015 |doi=10.3847/0004-637X/827/1/86 |volume=827 |issue=1 |journal=The Astrophysical Journal |page=86 |bibcode=2016ApJ...827...86K |s2cid=55162101 |doi-access=free}}</ref> This planet is located within the [[habitable zone]] of [[binary star system]] [[Kepler-1647]] and thus could theoretically have a [[Habitability of natural satellites|habitable]] Earth-like [[exomoon]].<ref>{{cite journal |last1=Barbosa |first1=G O |last2=Winter |first2=O C |last3=Amarante |first3=A |last4=Macau |first4=E E N |title=Formation of Earth-sized planets within the Kepler-1647 system habitable zone |journal=Monthly Notices of the Royal Astronomical Society |date=2021-05-25 |volume=504 |issue=4 |pages=6144–6156 |doi=10.1093/mnras/stab1165|doi-access=free |arxiv=2104.11628}}</ref>
|-
| style="border:4px ridge red; background:#000000; text-align:center;" |[[File:Kepler-90 h and hypothetical exomoon.jpg|112px]]
| [[Kepler-90h]]
| data-sort-value="1.01"|1.01 ± 0.09<ref name="NASAExoplanet" />
| style="text-align:center;" |←
| data-sort-value="0.639"|0.639 ± 0.016<ref name="Liang2020" />
| Located in the [[Kepler-90#Planetary system|Kepler-90 system]] with eight known exoplanets, whose [[Planetary system#System architectures|architecture]] is similar to that of the [[Solar System]], with [[rocky planet]]s being closer to the star and [[gas giant]]s being more distant. This planet is located at 1 [[astronomical unit|AU]] from its star, which is within the [[Kepler-90h#Habitability|habitable zone]] of [[Kepler-90]] and thus could theoretically have a [[Habitability of natural satellites|habitable]] Earth-like [[exomoon]].
|-
| style="border:4px ridge blue; background:#000000; text-align:center;"|[[File:WD 0806-661B NIRCam.jpg|112px]]
| [[Ahra]]<br />''(WD 0806-661 b)''
| data-sort-value="1.007"|1.007 – 1.04<ref name=Dupuy2013>{{Cite journal |last1=Dupuy |first1=Trent J. |last2=Kraus |first2=Adam L. |date=2013-09-27 |title=Distances, Luminosities, and Temperatures of the Coldest Known Substellar Objects |url=https://doi.org/10.1126/science.1241917 |arxiv=1309.1422 |journal=Science |volume=341 |issue=6153 |pages=1492–1495 |doi=10.1126/science.1241917 |pmid=24009359 |bibcode=2013Sci...341.1492D |issn=0036-8075}}</ref>
| style="text-align:center;" |←
| data-sort-value="6.8"|6.8 – 9.0<ref name=Dupuy2013 />
| First exoplanet discovered around a single (as opposed to [[Binary star|binary]]) [[white dwarf]], and the coldest directly imaged exoplanet when discovered.<ref name="qmDOD" /><br />Possibly formed closer to [[WD 0806−661|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 {{val|2500|ul=AU}}.<br />Might be considered an [[exoplanet]] or a [[sub-brown dwarf]], the [[Brown dwarf#Table of extremes|dimmest]] [[sub-brown dwarf]]. The [[International Astronomical Union|IAU]] considers objects below the {{val|p=~|13|ul=Jupiter mass}} limiting mass for [[deuterium fusion]] that orbit stars (or [[stellar remnants]]) to be planets, regardless on how they formed.<ref name="IAUplanetdef" />
|- style="background:pink;" 
|style="border:4px ridge cyan; background:#000000; text-align:center;"|[[File:Jupiter Earth Moon Comparison.png|112px]]
| [[Jupiter]]
| data-sort-value="1"|1<br />({{val|11.209|ul=Earth radius}})<ref name="Prša-2016" /><br />''[[Jupiter radius|(71 492 km)]]''
| style="text-align:center;" |{{number sign}}
| data-sort-value="1"|1<br />({{val|317.827|ul=Earth mass}})<ref name="JPL Planets" /><br />''[[Jupiter mass|(1.898 125 × 10<sup>27</sup> kg)]]''
| [[Jupiter#Formation and migration|Oldest]], largest and most massive [[Solar System planets|planet]] in the [[Solar System]];<ref name=":1" /> this planet hosts [[Moons of Jupiter|95 known moons]] including the [[Galilean moons]].<br /><small>''Reported for reference.''</small>
|-class="sortbottom" 
| colspan="6" | For smaller exoplanets, see the [[list of smallest exoplanets]] or other [[Lists of planets|lists of exoplanets]]. For exoplanets with milestones, see the [[list of exoplanet extremes]] and [[list of exoplanet firsts]].
|}

=== Notes ===
{{notelist}}

==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.<br /><small>'''Note: Some data may be unreliable or incorrect due to unit or conversion errors'''</small>
<div style=display:inline-grid>
{| class="wikitable" style="margin:0px 15px 0px 0px"
|+Key (Classification)
|-
| style="text-align:center;"| ←
! Probably planets (≲ 13 {{Jupiter mass|link=y}}) (based on mass)
|-
| bgcolor="#FE9F9F" style="text-align:center;"| ‡
! Unclassified object (unknown mass)
|-
| bgcolor="#e6e6e6" width=50px style="text-align:center;"| –
! Theoretical planet size restrictions
|}
</div>
<div style=display:inline-grid>
{| class="wikitable"
|+Key (Illustration)
|-
| style="border:4px ridge red;"|
! Artist's impression
|-
| style="border:4px ridge green;"|
! Composite image of direct observations
|}
</div>
{{sticky header}}
{| class="wikitable sortable sticky-header"
|-
! class="unsortable"| Illustration
! Name<br />''(Alternates)''<br /><small>''(Status)''</small>
! data-sort-type=number| Radius<br />({{Jupiter radius|link=y}})
! class="unsortable"| Key
! data-sort-type=number| Mass<br />({{Jupiter mass|link=y}})
! class="unsortable" | Notes
|-style="background:#e6e6e6"
|style="border:4px ridge red; background:#000000; text-align:center;"|[[File:Planet formation.jpg|112x112px]]
| ''[[Nebular hypothesis#Giant planets|New born planet]] limit''
| data-sort-value="30"|~ 30<ref name=":16">{{Cite journal |last1=Nayakshin |first1=Sergei |last2=Elbakyan |first2=Vardan |date=2024-01-23 |title=On the origin of accretion bursts in FU Ori |url=https://academic.oup.com/mnras/article/528/2/2182/7513777 |journal=Monthly Notices of the Royal Astronomical Society |language=en |volume=528 |issue=2 |pages=2182–2198 |arxiv=2309.12072 |bibcode=2024MNRAS.528.2182N |doi=10.1093/mnras/stae049 |issn=0035-8711 |doi-access=free}}</ref>
| style="text-align:center;"|–
| data-sort-value="20"|≤ 20<br />{{nowrap|(≤ 13)}}<ref name=":16" />
| Theoretical size limit of a newly-formed planet.
|-style="background:#e6e6e6"
|style="border:4px ridge red; background:#000000; text-align:center;"|[[File:Artist’s impression of an ultra-hot Jupiter transiting its star.jpg|112x112px]]
| ''Young [[Hot Jupiter]] limit''
| data-sort-value="20"|~ 20<ref name=":15">{{Cite journal |last1=Nayakshin |first1=Sergei |last2=Owen |first2=James E |last3=Elbakyan |first3=Vardan |date=2023-05-23 |title=Extreme evaporation of planets in hot thermally unstable protoplanetary discs: the case of FU Ori |url=https://academic.oup.com/mnras/article/523/1/385/7161140 |journal=Monthly Notices of the Royal Astronomical Society |language=en |volume=523 |issue=1 |pages=385–403 |arxiv=2305.03392 |bibcode=2023MNRAS.523..385N |doi=10.1093/mnras/stad1392 |issn=0035-8711 |doi-access=free}}</ref>
| style="text-align:center;"|–
| data-sort-value="10"|≤ 10<ref name=":15" />
| Theoretical size limit of a newly-formed planet that needed 10<sup>4</sup> – 10<sup>5</sup> ({{val|10000}} – {{val|100000}}) years to migrate close to the host star, but has not yet interacted with it beforehand.
|-
|style="border:4px ridge green; background:white; text-align:center;"|[[File:FUOriLightCurve.png|112px]]
| {{nowrap|[[FU Orionis|FU Orionis North b]]}}<br />''(FU Ori Ab)''<br /><var><small>(unconfirmed)</small></var>
| data-sort-value="10"|~ 9.8<ref name=":16" /><br />(~ {{val|1.0|ul=Solar radius}})
| style="text-align:center;" |←
| data-sort-value="3"|~ 3<ref name=":16" />
| Discovered using a variation of disk kinematics.<ref>{{Cite web |last= |first= |date= |title=Planet FU Ori b |url=https://exoplanet.eu/catalog/fu_ori_b--9413/ |access-date=2024-10-11 |website=Encyclopaedia of exoplanetary systems / exoplanet.eu |language=en}}</ref> [[Tidal disruption]] and extreme evaporation made the planet radius shrink from the beginning of the burst ({{Jupiter radius|14}}) in 1937<ref name=":15" /> to the present year by ~30 per cent and its mass is around half of its initial mass of {{Jupiter mass|6}}.<ref name=":15" /><ref name=":16" />
|- bgcolor="#FE9F9F"
|
| [[UCAC4 174-179953 b]]<br /><small>''(unclassified)''</small>
| 8.14 ± 0.40<ref name=":28">{{Cite journal |last1=Mékarnia |first1=D. |last2=Guillot |first2=T. |last3=Rivet |first3=J.-P. |last4=Schmider |first4=F.-X. |last5=Abe |first5=L. |last6=Gonçalves |first6=I. |last7=Agabi |first7=A. |last8=Crouzet |first8=N. |last9=Fruth |first9=T. |last10=Barbieri |first10=M. |last11=Bayliss |first11=D. D. R. |last12=Zhou |first12=G. |last13=Aristidi |first13=E. |last14=Szulagyi |first14=J. |last15=Daban |first15=J.-B. |date=2016-11-21 |title=Transiting planet candidates with ASTEP 400 at Dome C, Antarctica |journal=Monthly Notices of the Royal Astronomical Society |language=en |volume=463 |issue=1 |pages=45–62 |bibcode=2016MNRAS.463...45M |doi=10.1093/mnras/stw1934 |doi-access=free |issn=0035-8711}}</ref> <br />(0.84 {{Solar radius|link=y}})
| style="text-align:center;" |‡
| ''Unknown''
| rowspan="12" |Object cannot be classified as brown dwarf or exoplanet without a mass estimate.
|- bgcolor="#FE9F9F"
|
| [[UCAC4 220-040923 b]]<br /><small>''(unclassified)''</small>
| 4.65 ± 0.20<ref name=":28" />
| style="text-align:center;" |‡
| ''Unknown''
|- bgcolor="#FE9F9F"
|
| [[UCAC4 223-042828 b]]<br /><small>''(unclassified)''</small>
| 3.33 ± 0.50<ref name=":28" />
| style="text-align:center;" |‡
| ''Unknown''
|- bgcolor="#FE9F9F"
| 
| [[UCAC4 185-192986 b]]<br /><small>''(unclassified)''</small>
| 3.3 ± 0.2<ref name=":28" />
| style="text-align:center;" |‡
| ''Unknown''
|- bgcolor="#FE9F9F"
| 
| [[UCAC4 118-126574 b]]<br /><small>''(unclassified)''</small>
| 3.12 ± 0.10<ref name=":28" />
| style="text-align:center;" |‡
| ''Unknown''
|- bgcolor="#FE9F9F"
|
| [[UCAC4 171-187216 b]]<br /><small>''(unclassified)''</small>
| data-sort-value="2.751"|2.75 ± 0.20<ref name=":28" />
| style="text-align:center;" |‡
| ''Unknown''
|- bgcolor="#FE9F9F"
|
| [[KOI-7073 b]]<br /><small>''(unclassified)''</small>
| {{nowrap|2.699 {{±|0.473|0.794}}}}<ref>{{Cite web |title=The Extrasolar Planet Encyclopaedia — KOI-7073 b |url=https://exoplanet.eu/catalog/koi_7073_b--6240/ |website=[[Extrasolar Planets Encyclopaedia]]. [[Paris Observatory]]|date=2019}}</ref>
| style="text-align:center;" |‡
| data-sort-value="1.0011" |''Unknown''
|- bgcolor="#FE9F9F"
| 
| [[UCAC4 175-188215 b]]<br /><small>''(unclassified)''</small>
| 2.69 ± 0.50<ref name=":28" />
| style="text-align:center;" |‡
| ''Unknown''
|- bgcolor="#FE9F9F"
| 
| [[UCAC4 116-118563 b]]<br /><small>''(unclassified)''</small>
| 2.62 ± 0.10<ref name=":28" />
| style="text-align:center;" |‡
| ''Unknown''
|- bgcolor="#FE9F9F"
|
| [[19g-2-01326 b]]<br /><small>''(unclassified)''</small>
| {{nowrap|2.29 {{±|0.13|0.61}}}}<ref>{{Cite web |title=The Extrasolar Planet Encyclopaedia — 19g-2-01326 b |url=https://exoplanet.eu/catalog/19g_2_01326_b--1230/ |website=[[Extrasolar Planets Encyclopaedia]]. [[Paris Observatory]]|date=2013}}</ref>
| style="text-align:center;" |‡
| ''Unknown''
|- bgcolor="#FE9F9F"
| 
| [[SOI-2 b]]<br /><small>''(unclassified)''</small>
| data-sort-value="2.22"|2.22<ref name=":30">{{Cite journal |last1=Yakovlev |first1=O. Ya. |last2=Valeev |first2=A. F. |last3=Valyavin |first3=G. G. |last4=Tavrov |first4=A. V. |last5=Aitov |first5=V. N. |last6=Mitiani |first6=G. Sh. |last7=Beskin |first7=G. M. |last8=Korablev |first8=O. I. |last9=Galazutdinov |first9=G. A. |last10=Vlasyuk |first10=V. V. |last11=Emelyanov |first11=E. V. |last12=Fatkhullin |first12=T. A. |last13=Sasyuk |first13=V. V. |last14=Perkov |first14=A. V. |last15=Bondar’ |first15=S. F. |date=March 2023 |title=Eight Exoplanet Candidates in SAO Survey |url=https://link.springer.com/10.1134/S1990341323010108 |journal=Astrophysical Bulletin |language=en |volume=78 |issue=1 |pages=79–93 |arxiv=2304.01076 |bibcode=2023AstBu..78...79Y |doi=10.1134/S1990341323010108 |issn=1990-3413}}</ref>
| style="text-align:center;" |‡
| data-sort-value="1.001" |''Unknown''
|- bgcolor="#FE9F9F"
|
| [[TIC 332350266.01]]<br /><small>''(unclassified)''</small>
| data-sort-value="2.21"|2.21{{±|3.18}}<ref name=":29" />
| style="text-align:center;" |‡
| ''Unknown''
|- style="background:#e6e6e6" 
|style="border:4px ridge red; background:#000000; text-align:center;"|[[File:Artist’s impression of an ultra-hot Jupiter transiting its star.jpg|112x112px]]
| ''Old [[Hot Jupiter]] limit''
| data-sort-value="2.2"|2.2<ref name="limit" />
| style="text-align:center;" |–
| data-sort-value="0.0000000000000000001"|> 0
| Theoretical limit for [[hot Jupiter]]s close to a star, that are limited by [[tidal heating]], resulting in 'runaway inflation'
|- bgcolor="#FE9F9F"
|
| [[TIC 138664795.01]]<br /><small>''(unclassified)''</small>
| 2.16 ± 0.16<ref name=":29" />
| style="text-align:center;" |‡
| ''Unknown''
| rowspan="16" |Object cannot be classified as brown dwarf or exoplanet without a mass estimate.
|- bgcolor="#FE9F9F"
|
| [[UCAC4 221-041868 b]]<br /><small>''(unclassified)''</small>
| 2.1 ± 0.20<ref name=":28" />
| style="text-align:center;" |‡
| ''Unknown''
|- bgcolor="#FE9F9F"
|
| [[TOI-496 b]]<br /><small>''(unclassified)''</small>
| 2.05 {{±|0.63|0.29}}<ref>{{Cite journal |last1=Nardiello |first1=D |last2=Piotto |first2=G |last3=Deleuil |first3=M |last4=Malavolta |first4=L |last5=Montalto |first5=M |last6=Bedin |first6=L R |last7=Borsato |first7=L |last8=Granata |first8=V |last9=Libralato |first9=M |last10=Manthopoulou |first10=E E |date=2020-07-11 |title=A PSF-based Approach to TESS High quality data Of Stellar clusters (PATHOS) – II. Search for exoplanets in open clusters of the Southern ecliptic hemisphere and their frequency |url=https://academic.oup.com/mnras/article/495/4/4924/5850378 |journal=Monthly Notices of the Royal Astronomical Society |language=en |volume=495 |issue=4 |pages=4924–4942 |arxiv=2005.12281 |bibcode=2020MNRAS.495.4924N |doi=10.1093/mnras/staa1465 |doi-access=free |issn=0035-8711}}</ref>
| style="text-align:center;" |‡
| ''Unknown''
|- bgcolor="#FE9F9F"
|
| [[SOI-7 b]]<br /><small>''(unclassified)''</small>
| data-sort-value="1.96"| 1.96<ref name=":30" />
| style="text-align:center;" |‡
| data-sort-value="1.0009" |''Unknown''
|- bgcolor="#FE9F9F"
|
| [[UCAC4 121-140615 b]]<br /><small>''(unclassified)''</small>
| 1.94 ± 0.20<ref name=":28" />
| style="text-align:center;" |‡
| ''Unknown''
|- bgcolor="#FE9F9F"
|
| [[UCAC4 123-150641 b]]<br /><small>''(unclassified)''</small>
| 1.93 ± 0.20<ref name=":28" />
| style="text-align:center;" |‡
| ''Unknown''
|- bgcolor="#FE9F9F"
|
| [[TIC 274508785.01]]<br /><small>''(unclassified)''</small>
| 1.92{{±|2.37}}<ref name=":29" />
| style="text-align:center;" |‡
| ''Unknown''
|- bgcolor="#FE9F9F"
|
| [[W74 b]]<br />''(Gaia DR2 6045477635223138432 b)'' <br /><small>''(unclassified)''</small>
| 1.9<ref>{{Cite journal |last1=Wallace |first1=Joshua J. |last2=Hartman |first2=Joel D. |last3=Bakos |first3=Gáspár Á. |date=2020-03-01 |title=A Search for Transiting Planets in the Globular Cluster M4 with K2: Candidates and Occurrence Limits |journal=The Astronomical Journal |volume=159 |issue=3 |pages=106 |arxiv=2001.08362 |bibcode=2020AJ....159..106W |doi=10.3847/1538-3881/ab66b4 |doi-access=free |issn=0004-6256}}</ref>
| style="text-align:center;" |‡
| ''Unknown''
|- bgcolor="#FE9F9F"
|
| [[TIC 116307482.01]] <br /><small>''(unclassified)''</small>
| 1.89 ± 1.46<ref name=":29" />
| style="text-align:center;" |‡
| ''Unknown''
|- bgcolor="#FE9F9F"
|
| [[UCAC4 122-142653 b]]<br /><small>''(unclassified)''</small>
| 1.85 ± 0.10<ref name=":28" />
| style="text-align:center;" |‡
| data-sort-value="1.0007" |''Unknown''
|- bgcolor="FE9F9F"
|
| [[TIC 77173027.01]]<br /><small>''(unclassified)''</small>
| 1.84 ± 1.12<ref name=":29" />
| style="text-align:center;" |‡
| data-sort-value="1.0006" |''Unknown''
|- bgcolor="#FE9F9F"
|
| [[TOI-159 Ab]]<br /><small>''(unclassified)''</small>
| data-sort-value="1.81"|1.80 ± 0.77<ref>{{Cite journal |last1=Lester |first1=Kathryn V. |last2=Howell |first2=Steve B. |last3=Ciardi |first3=David R. |last4=Matson |first4=Rachel A. |date=2022-08-01 |title=Determining Which Binary Component Hosts the TESS Transiting Planet |journal=The Astronomical Journal |volume=164 |issue=2 |pages=56 |arxiv=2206.02825 |bibcode=2022AJ....164...56L |doi=10.3847/1538-3881/ac75ee |doi-access=free |issn=0004-6256}}</ref>
| style="text-align:center;" |‡
| data-sort-value="1.0003" |''Unknown''
|- bgcolor="#FE9F9F"
|
| [[TIC 82205179.01]]<br />''(TIC 82205179 b)''<br /><small>''(unclassified)''</small>
| 1.76 ± 0.56<ref name=":29">{{Cite journal |last1=Nguyen |first1=Kendra T. |last2=Caldwell |first2=Douglas A. |last3=Twicken |first3=Joseph D. |last4=Striegel |first4=Stephanie L. |last5=Ting |first5=Eric B. |last6=Williams |first6=Rosemary H. |last7=Jenkins |first7=Jon M. |date=October 2022 |title=Release of TESS Objects of Interest from TESS-SPOC Sectors 48 to 50 Full Frame Images |journal=Research Notes of the AAS |language=en |volume=6 |issue=10 |pages=207 |doi=10.3847/2515-5172/ac983a |doi-access=free |bibcode=2022RNAAS...6..207N |issn=2515-5172}}</ref>
| style="text-align:center;" |‡
| data-sort-value="0.00009"|''Unknown''
|- bgcolor="#FE9F9F"
|
| [[UCAC4 124-144273 b]]<br /><small>''(unclassified)''</small>
| 1.71 ± 0.10<ref name=":28" />
| style="text-align:center;" |‡
| data-sort-value="1.00007" |''Unknown''
|- bgcolor="#FE9F9F"
|
| [[TOI-710 b]]<br /><small>''(unclassified)''</small>
| 1.66 ± 1.10<ref name=Bass-2024-26-11>{{cite arXiv |last1=Bass |first1=Dillon |last2=Fabrycky |first2=Daniel |title=Validating the Orbital Periods of the Coolest TESS Exoplanet Candidates |date=2024-11-26 |class=astro-ph.EP |eprint=2411.17640}}</ref>
| style="text-align:center;" |‡
| data-sort-value="1.00007" |''Unknown''
|-
|}

===Exoplanets with uncertain radii===
This list contains planets with uncertain radii that could be below or above the adopted cut-off of {{jupiter radius|1.6}}, depending on the estimate.

<div style=display:inline-grid>
{| class="wikitable" style="margin:0px 15px 0px 0px"
|+Key (classification)
|-
| style="text-align:center;"| ←
! Probably planets (≲ 13 {{Jupiter mass|link=y}}) (based on mass)
|-
| bgcolor="#cff7c1" width=50px style="text-align:center;"|?
! Status uncertain (inconsistency in age or mass of planetary system)
|-
| bgcolor="#CEE0F2" width="50px" style="text-align:center;" | →
! Planets with grazing transit, hindering radius determination
|}
</div>
<div style=display:inline-grid>
{| class="wikitable"
|+Key (illustration)
|-
| style="border:4px ridge blue;"|
! Direct imaging telescopic observation
|}
</div>
{{sticky header}}
{| class="wikitable sortable sticky-header"
! class="unsortable"| Illustration
! Name<br />''(Alternates)''
! data-sort-type=number| Radius <br />({{Jupiter radius|link=y}})
! class="unsortable"| Key
! data-sort-type=number| Mass <br />({{Jupiter mass|link=y}})
! class="unsortable"| Notes
|-
| style="border:4px ridge blue; background:#000000; text-align:center;"| [[File:The Star AB Pictoris and its Companion - Phot-14d-05-normal.jpg|112x112px]]
| [[AB Pictoris b]]<br />''(AB Pic b)''
| data-sort-value="1.57"|1.57 ± 0.07{{snd}}1.8 ± 0.3<ref name="Palma-Bifani-2023" />
| style="text-align:center;" |←
| data-sort-value="10"|10 ± 1<ref name="Palma-Bifani-2023" />
|{{nowrap| Previously believed to be a likely brown dwarf, with}} mass estimates of {{val|13|-|14|u=Jupiter mass}}<ref name="chauvin" /> to {{val|70|u=Jupiter mass}},<ref name="neu05" /> its mass is now estimated to be {{Val|10|1|u=Jupiter mass}}, with an age of {{val|13.0|1.1|0.6}} million years.<ref name="Palma2022" />
|- style="background:#CEE0F2" 
|
| [[TOI-2193 Ab]]
| data-sort-value="1.55" |>{{nowrap|1.55 (95% lower limit)}}<ref name="Yee-2022" />
| style="text-align:center;" | →
| data-sort-value="0.94" |{{nowrap|0.94 ± 0.18}}<ref name="Yee-2022" />
| Grazing planet, a large reported radius of {{Jupiter radius|1.77}} is unreliable. Whether it is larger than {{Jupiter radius|1.6}} is unknown.
|- style="background:#CEE0F2" 
|
| [[TOI-3540 b]]
| data-sort-value="1.44" | >1.44 (95% lower limit)<ref name="Yee-2022" />
| style="text-align:center;" | →
| data-sort-value="1.18" |1.18 ± 0.14<ref name="Yee-2022" />
| Grazing planet, a large reported radius of {{Jupiter radius|2.10}} is unreliable. Whether it is larger than {{Jupiter radius|1.6}} is unknown.
|- style="background:#CEE0F2" 
|
| [[TOI-1408 b]]
| data-sort-value="2.23"|>1, 1.5 (estimate),<ref name=Galazutdinov2023 /><br />2.23 ± 0.36,{{Efn|1=Converted from {{val|25|4|ul=Earth radius}}.}}<br />2.4 ± 0.5<ref name="Korth-2024" />
| style="text-align:center;" | →
| data-sort-value="1.86"|1.86 ± 0.02<ref name="Korth-2024" />
| A large radius of {{val|2.23|-|2.4|u=Jupiter radius}} has been derived from transit photometry,<ref name="Korth-2024" /> 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 {{jupiter radius|1}} can be obtained, whether TOI-1408 b is larger than {{Jupiter radius|1.6}} is unknown.<ref name=Galazutdinov2023 />
|}

=== Notes ===
{{notelist}}

== Chronological list of largest exoplanets ==
These exoplanets were the largest at the time of their discovery.
<div style="display:inline-grid">
{| class="wikitable" style="margin:0px 15px 0px 0px"
|+Key (classification)
|-
| bgcolor="#FFF8DC" width="50px" style="text-align:center;" |{{asterisk}}
! Later identified to be a probable/confirmed brown dwarf (≳ 13 {{Jupiter mass}}) or a star (≳ 82.76 {{Jupiter mass}})
|-
| bgcolor="#CEF2E0" width="50px" style="text-align:center;" |{{dagger}}
! Candidate for largest exoplanet (currently or in time span)
|-
| bgcolor="#CFF7C1" width=50px style="text-align:center;"|?
! Status uncertain (inconsistency in age or mass of planetary system) while being candidate for largest exoplanet
|-
| bgcolor="#CEE0F2" width="50px" style="text-align:center;" | →
! Assumed largest exoplanet, while unconfirmed, later retracted or later confirmed
|-
| style="text-align:center;" | ←
! Largest exoplanet (≲ 13 {{Jupiter mass}}) at the time
|-
| bgcolor="#e6e6e6" width="50px" style="text-align:center;" | –
! Largest confirmed exoplanet (in radius and mass), while discovered candidates might be larger
|-
| bgcolor="pink" width="50px" style="text-align:center;" |{{number sign}}
! Non-exoplanets reported for reference
|}
</div>
<div style="display:inline-grid">
{| class="wikitable"
|+Key (illustration)
|-
| style="border:4px ridge red;" |
! Artist's impression
|-
| style="border:4px ridge orange;"|
! Artist's impression size comparison
|-
| style="border:4px ridge blue;" |
! Direct Imaging telescopic observation
|-
| style="border:4px ridge purple;" |
! Transiting telescopic observation
|-
| style="border:4px ridge pink;" |
! Graphic chart
|}
</div>
{{sticky header}}
{| class="wikitable sortable sticky-header"
|-
! data-sort-type=number| Years largest discovered
! class="unsortable"| Illustration
! Name<br />''(Alternates)''
! data-sort-type=number| Radius <br />({{Jupiter radius|link=y}})
! class="unsortable"| Key
! data-sort-type="number" | Mass <br />({{Jupiter mass|link=y}})
! class="unsortable" | Notes
|- style="background:#e6e6e6"
| data-sort-value="2024" |2024{{snd}}present
| style="border:4px ridge orange; background:#000000;" |[[File:Comparison XO-6.png|112x112px]]
| [[XO-6b]] 
| data-sort-value="2.171" |2.17 ± 0.2<ref name="Saha2024" />
| style="text-align:center;" | –
| data-sort-value="4.472" |4.47 ± 0.12<ref name="Saha2024" />
| A very puffy [[Hot Jupiter]]
|- style="background:#CEF2E0"
| data-sort-value="2024" |(2024{{snd}}2024)
| style="border:4px ridge blue; background:#000000;" |[[File:ROXs 42B MUSE IR.jpg|112x112px]]
| [[ROXs 42Bb|ROXs 42B b]]
| data-sort-value="2.10" |2.10 ± 0.35<ref name="Xuan-2024" />
| style="text-align:center;" | {{dagger}}
| data-sort-value="9.001" |9 {{±|6|3}};<ref name=":12" /> 10 ± 4<ref name=":13" />
|Large size needs confirmation. Other estimates include 1.9 – 2.4 {{Jupiter radius|link=y}}, 1.3{{Snd}}4.7 {{Jupiter radius}}.<ref name="DaemgenROX" /> Other recent sources of masses include 3.2 – 27 {{Jupiter mass|link=y}},<ref name="Inglis2024" /> 13 ± 5 {{Jupiter mass|link=y}}.<ref name="Xuan-2024" />
|- style="background:#e6e6e6"
| data-sort-value="2024" |2024 – 2024
| style="border:4px ridge purple; background:#000000; "|[[File:Transit light curve of Hat-P-67b.png|112x112px]]
| [[HAT-P-67b]]
| 2.165 {{±|0.024|0.022}}{{efn|name=HatP67|Calculated using R<sub>p</sub>/R<sub>⋆</sub> multiplied by R<sub>⋆</sub>. The value is later multiplied by (142984 ''km'' ÷ 1391400 ''km'') to convert from {{solar radius|link=y}} to {{jupiter radius|link=y}}.}}<ref name=Gully-Santiago />
| style="text-align:center;" | –
| 0.418 ± 0.012<ref name=Saha2024 />
| A very puffy [[Hot Jupiter]]. Previously the largest known planet with an accurately and precisely measured radius,<ref name="largest" /> a new estimate revised its radius.<ref name="Gully-Santiago" /><ref name=Saha2024 />
|- style="background:#cff7c1"
| data-sort-value="2022" |(2022 – 2025)
| style="border:4px ridge blue; background: white; text-align:center;" |[[File:Subaru AB Aur b.png|112x112px]]
| [[AB Aurigae b]] <br />''(AB Aur b, <br />HD 31293 b)''
| data-sort-value="2.75" |2.75<ref name="Currie-2022" />
| style="text-align:center;" |?
| data-sort-value="20" |20 {{nowrap|(~ 4 [[Megayear|Myr]])}}<ref name="Ginski2022" /><br />< 130,<br />{{nowrap|10 – 12}} {{nowrap|(1 [[Megayear|Myr]])}}<ref name="Currie-2022" />
| 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,<ref name="Boss1997">{{Cite journal |title=Giant Planet Formation by Gravitational Instability |last1=Boss |first1=Alan |journal=Science |language=en |volume=276 |issue=5320 |pages=1836–1839 |date= June 1997 |bibcode=1997Sci...276.1836B |doi=10.1126/science.276.5320.1836}}</ref> where as a massive disk around a star cools, gravity causes the disk to rapidly break up into one or more planet-mass fragments.<ref name="hubblesite">{{cite web | title=Hubble Finds a Planet Forming in an Unconventional Way | website=HubbleSite.org | date=April 4, 2022 | url=http://hubblesite.org/contents/news-releases/2022/news-2022-016 | access-date=April 10, 2022}}</ref>
|- style="background:#CEF2E0"
| data-sort-value="2022" |(2022 – present)
| style="border:4px ridge blue; background:#000000;" rowspan="3" |[[File:PDS 70.jpg|112x112px]]
| rowspan="3" |[[PDS 70 b|PDS 70b]]
| 2.7<ref name="Zhou2022" />
| rowspan="3" style="text-align:center;" | {{dagger}}
| rowspan="3" |3.2 {{±|3.3|1.6}}, 7.9 {{±|4.9|4.7}},<br />< 10 (2 σ),<br />≲ 15 (total)<ref name="Wang 王-2021" />
| rowspan="3" |Has been later measured to have a radius of only {{Jupiter radius|1.96}},<ref name="Wang2021" /> and then {{jupiter radius|2.7}} in 2022.<ref name=Zhou2022 /> Large size needs confirmation due to this discrepancy.
|- style="background:#CEF2E0"
| data-sort-value="2021" |(2021 – 2022)
| 1.96<ref name="Wang2021" />
|- style="background:#CEF2E0"
| data-sort-value="2020" |(2020 – 2021)
| 2.09 {{±|0.23|0.31}}{{snd}}2.72 {{±|0.15|0.17}}<ref>{{Cite journal |last1=Wang 王劲 |first1=Jason J. 飞 |last2=Ginzburg |first2=Sivan |last3=Ren 任 |first3=Bin 彬 |last4=Wallack |first4=Nicole |last5=Gao |first5=Peter |last6=Mawet |first6=Dimitri |last7=Bond |first7=Charlotte Z. |last8=Cetre |first8=Sylvain |last9=Wizinowich |first9=Peter |last10=De Rosa |first10=Robert J. |last11=Ruane |first11=Garreth |last12=Liu |first12=Michael C. |last13=Absil |first13=Olivier |last14=Alvarez |first14=Carlos |last15=Baranec |first15=Christoph |date=2020-06-01 |title=Keck/NIRC2 L'-band Imaging of Jovian-mass Accreting Protoplanets around PDS 70 |journal=The Astronomical Journal |volume=159 |issue=6 |pages=263 |arxiv=2004.09597 |bibcode=2020AJ....159..263W |doi=10.3847/1538-3881/ab8aef |doi-access=free |issn=0004-6256}}</ref>
|- style="background:#CFF7C1"
| data-sort-value="2020" |(2020{{snd}}present)
| style="border:4px ridge blue; background:#000000;" |[[File:SR 12 C.jpg|112x112px]]
| [[SR 12 (star)|SR 12 c]]<br />''(SR 12 (AB) c,<br /> SR 12 C)''
| data-sort-value="2.38" |2.38 {{±|0.27|0.32}}<ref name="Bryan-2020" />
| style="text-align:center;" |?
| 13 ± 2<ref name="Bryan-2020" />
| 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}} {{Jupiter mass|link=y}},<ref name=":9" /> 12{{snd}}15 {{Jupiter mass|link=y}}.<ref name=":10" />
|- style="background:#e6e6e6"
| data-sort-value="2017.2" |2017 – 2024
| style="border:4px ridge purple; background:#000000; "|[[File:Transit light curve of Hat-P-67b.png|112x112px]]
| [[HAT-P-67b]]
| 2.085 {{±|0.096|0.071}}<ref name="Zhou2017HAT">{{Cite journal |last1=Zhou |first1=G. |last2=Bakos |first2=G. á. |last3=Hartman |first3=J. D. |last4=Latham |first4=D. W. |last5=Torres |first5=G. |last6=Bhatti |first6=W. |last7=Penev |first7=K. |last8=Buchhave |first8=L. |last9=Kovács |first9=G. |last10=Bieryla |first10=A. |last11=Quinn |first11=S. |last12=Isaacson |first12=H. |last13=Fulton |first13=B. J. |last14=Falco |first14=E. |last15=Csubry |first15=Z. |date=2017-05-01 |title=HAT-P-67b: An Extremely Low Density Saturn Transiting an F-subgiant Confirmed via Doppler Tomography ∗ |journal=The Astronomical Journal |volume=153 |issue=5 |pages=211 |arxiv=1702.00106 |bibcode=2017AJ....153..211Z |doi=10.3847/1538-3881/aa674a |doi-access=free |issn=0004-6256}}</ref>
| style="text-align:center;" | –
| 0.34 {{±|0.25|0.19}}<ref name="Zhou-2017" />
| A very puffy [[Hot Jupiter]]. At discovery the largest known planet with an accurately and precisely measured radius.<ref name="largest" />
|- style="background:#e6e6e6"
| data-sort-value="2017" |2017 – 2017
| style="border:4px ridge orange; background:#000000;" |[[File:Comparison XO-6.png|112x112px]]
| [[XO-6b]] 
| 2.07 ± 0.22<ref name="zhao" />
| style="text-align:center;" | –
| 4.47 ± 0.12<ref name="Saha2024" />
| A very puffy [[Hot Jupiter]]
|- style="background:#CEF2E0"
| data-sort-value="2014" |(2014{{snd}}2024)
| style="border:4px ridge blue; background:#000000;" |[[File:ROXs 42B MUSE IR.jpg|112x112px]]
| [[ROXs 42Bb|ROXs 42B b]]
| data-sort-value="2.43" |2.43 ± 0.18 – 2.55 ± 0.2<ref name=":14" />
| style="text-align:center;" | {{dagger}}
| 9 {{±|6|3}};<ref name=":12" /> 10 ± 4<ref name=":13" />
|Large size needs confirmation. Other estimates include 1.9 – 2.4 {{Jupiter radius|link=y}}, 1.3{{Snd}}4.7 {{Jupiter radius}}.<ref name="DaemgenROX" />
|- style="background:#CEF2E0"
| data-sort-value="2014.1" |(2014{{snd}}present)
| style="border:4px ridge blue; background:#000000;" |[[File:DH Tauri.jpg|112x112px]]
| [[DH Tauri b]]<br />''(DH Tau b)''
| data-sort-value="2.7" |2.7 ± 0.8<ref name="zhou2014" /> 
| style="text-align:center;" | {{dagger}}
| data-sort-value="11.5001" |11.5 {{±|10.5|3.1}}<ref name=":22" />
| Mass being below the deuterium burning limit needs confirmation. Temperature originally given as 2700 – 2800 K.<ref name=":23" /> Other sources give the radii: 2.49 {{Jupiter radius|link=y}},<ref name="Bonnefoy-2014" />{{efn|name=L/Teff|Based on the estimated temperature and luminosity via the [[Stefan-Boltzmann law]].}} 2.68 {{Jupiter radius|link=y}},<ref name="Xuan-2020" /> and 2.6 ± 0.6 {{Jupiter radius|link=y}}<ref name="Xuan-2024" /> and masses: 11 ± 3 {{Jupiter mass|link=y}},<ref name="zhou2014" /> 14.2 {{±|2.4|3.5}} {{Jupiter mass|link=y}},<ref name=":5" /> 17 ± 6 {{Jupiter mass|link=y}}<ref name=":6" /> and 12 ± 4 {{Jupiter mass|link=y}}<ref name="Xuan-2024" />
|- style="background:#e6e6e6"
| data-sort-value="2010" |2010{{snd}}2017
| style="border:4px ridge red; background:#000000; text-align:center;" | [[File:WASP-17b.jpg|112x112px]]
| [[WASP-17b|Ditsö̀]] <br />''(WASP-17b)''
| 1.74 {{±|0.26|0.23}}<ref name="Anderson2010" />
| style="text-align:center;" | –
| 0.512 ± 0.037<ref name="Bonomo-2017b" />
| First planet discovered to have a [[retrograde orbit]]<ref name="Anderson2010" /> and first to have [[quartz]] (crystalline silica, SiO<sub>2</sub>) in the clouds of an exoplanet.<ref name="Quartz" /> Puffiest and possibly largest exoplanet at the time of discovery.<ref name="BP" /> {{nowrap|Extremely low density of 0.08 g/cm<sup>3</sup>.}}<ref name=":3" />
|- style="background:#e6e6e6"
| data-sort-value="2007" |2007{{snd}}2010
| style="border:4px ridge orange; background:#000000;" |[[File:TrES-4.jpg|112x112px]]
| [[TrES-4b|TrES-4]]<br />''(GSC 02620-00648 Ab)''
| 1.674 ± 0.094<ref>{{Cite journal |last1=Mandushev |first1=Georgi |last2=O'Donovan |first2=Francis T. |last3=Charbonneau |first3=David |last4=Torres |first4=Guillermo |last5=Latham |first5=David W. |last6=Bakos |first6=Gáspár Á. |last7=Dunham |first7=Edward W. |last8=Sozzetti |first8=Alessandro |last9=Fernández |first9=José M. |last10=Esquerdo |first10=Gilbert A. |last11=Everett |first11=Mark E. |last12=Brown |first12=Timothy M. |last13=Rabus |first13=Markus |last14=Belmonte |first14=Juan A. |last15=Hillenbrand |first15=Lynne A. |date=2007-10-01 |title=TrES-4: A Transiting Hot Jupiter of Very Low Density |url=https://iopscience.iop.org/article/10.1086/522115 |journal=The Astrophysical Journal |language=en |volume=667 |issue=2 |pages=L195–L198 |arxiv=0708.0834 |bibcode=2007ApJ...667L.195M |doi=10.1086/522115 |issn=0004-637X}}</ref>
| style="text-align:center;" | –
| data-sort-value="0.78"|0.78 ± 0.19<ref name="Stassun-2017" /><ref name="Johns" />
| This planet has a density of 0.2 g/cm<sup>3</sup>, less than [[Saturn#Internal structure|Saturn's]] 0.7 g/cm<sup>3</sup>.
|- style="background:#FFF8DC"
| data-sort-value="2007"|(2007{{snd}}present)
|style="border:4px ridge blue; background:#000000; text-align:center;"|[[File:The Sub-Stellar Companion to GQ Lupi.jpg|112x112px]]
| [[GQ Lupi b]] <br />''(GQ Lup Ab, <br />GQ Lup B)''
| data-sort-value="3.50"|3.50 {{±|1.50|1.03}}<ref name="Seifahrt07" />
| style="text-align:center;" | *
| data-sort-value="1.002"|1 – 46<ref name="R.Neuhäuser" />
| First confirmed [[exoplanet|exoplanet candidate]] to be directly imaged. <!-- 2M1207 b was confirmed few months later --> 
|- style="background:#CEF2E0"
| data-sort-value="2006.5" |(2006{{snd}}2014)
| style="border:4px ridge blue; background:#000000;" |[[File:DH Tauri.jpg|112x112px]]
| [[DH Tauri b]]<br />''(DH Tau b)''
| data-sort-value="1.75" |1.75<ref name=":22" /><ref name=":23" />{{efn|name=L/Teff|Based on the estimated temperature and luminosity via the [[Stefan-Boltzmann law]].}}
| style="text-align:center;" | {{dagger}}
| data-sort-value="11.5" |11.5 {{±|10.5|3.1}}<ref name=":22" />
| Mass being below the deuterium burning limit needs confirmation. Temperature originally given as 2700 – 2800 K.<ref name=":23" />
|- style="background:#e6e6e6"
| data-sort-value="2006"|2006{{snd}}2007
| style="border:4px ridge red; background:black; text-align:center; margin:0 0 12px 0; "|[[File:Osiris (HD209458b) planet illustration.jpeg|112x112px]]
| [[HD 209458 b]]<br />''("Osiris")''
| data-sort-value="1.275"|1.27 ± 0.02<ref name="iopscience.iop.org">{{Cite journal |last1=Charbonneau |first1=David |last2=Brown |first2=Timothy M. |last3=Latham |first3=David W. |last4=Mayor |first4=Michel |date=2000-01-20 |title=Detection of Planetary Transits Across a Sun-like Star |url=https://iopscience.iop.org/article/10.1086/312457 |journal=The Astrophysical Journal |volume=529 |issue=1 |pages=L45–L48 |arxiv=astro-ph/9911436 |bibcode=2000ApJ...529L..45C |doi=10.1086/312457|pmid=10615033}}</ref>
| style="text-align:center;" | –
| data-sort-value="0.6825" |0.682 {{±|0.014|0.015}}<ref name="Bonomo-2017a" />
| First known [[transiting exoplanet]], first precisely measured planet available, first to have its orbital speed measured, determining its mass directly,<ref name="Ignas" /> one of first two exoplanets (other being [[HD 189733 Ab]]) to be observed [[Spectroscopy|spectroscopically]]<ref name="Spectroscopy" /><ref name="Richardson2007" /> 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".''
|- style="background:#CEF2E0"
| data-sort-value="2005"|(2005{{snd}}2007)
|style="border:4px ridge blue; background:#000000; text-align:center;"|[[File:The Sub-Stellar Companion to GQ Lupi.jpg|112x112px]]
| [[GQ Lupi b]] <br />''(GQ Lup Ab, <br />GQ Lup B)''
| data-sort-value="2"|~ 2<ref>{{Cite journal |last1=Neuhäuser |first1=R. |last2=Guenther |first2=E. W. |last3=Wuchterl |first3=G. |last4=Mugrauer |first4=M. |last5=Bedalov |first5=A. |last6=Hauschildt |first6=P. H. |date=May 2005 |title=Evidence for a co-moving sub-stellar companion of GQ Lup |url=http://www.aanda.org/10.1051/0004-6361:200500104 |journal=Astronomy & Astrophysics |volume=435 |issue=1 |pages=L13–L16 |arxiv=astro-ph/0503691 |bibcode=2005A&A...435L..13N |doi=10.1051/0004-6361:200500104 |issn=0004-6361}}</ref>
| style="text-align:center;" | {{dagger}}
| data-sort-value="1.001"|1 – 46<ref name="R.Neuhäuser" />
| First confirmed [[exoplanet|exoplanet candidate]] to be directly imaged. <!-- 2M1207 b was confirmed few months later --> 
|-
| data-sort-value="1999"|1999{{snd}}2006
| style="border:4px ridge purple; background:white; text-align:center;"|[[File:V376PegLightCurve.png|112x112px]]
| [[HD 209458 b]]<br />''("Osiris")''
| 1.27 ± 0.02<ref name="iopscience.iop.org" />
| style="text-align:center;" | ←
| data-sort-value="0.682" |0.682 {{±|0.014|0.015}}<ref name="Bonomo-2017a" />
| First known [[transiting exoplanet]], first precisely measured radius available, first to have its orbital speed measured, determining its mass directly,<ref name="Ignas" /> 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".''
|- style="background:#CEF2E0"
| data-sort-value="1996"|(1995{{snd}}1999)
| style="border:4px ridge pink; background:#000000;" |[[File:ExoplanetPopulations-20170616.png|112x112px]]
| [[List of exoplanets discovered before 2000|various]]
| data-sort-value="1.01"|''Unknown''
| style="text-align:center;" | {{dagger}}
| data-sort-value="0.49"|[[HD 75289 b|0.49]]{{snd}}[[HD 222582 b|8.37]]
| About 20{{snd}}25 [[List of exoplanets discovered before 2000|planets]] including [[Upsilon Andromedae b|Saffar]] were found within this time span via the [[Doppler spectroscopy|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.
|- style="background:#e6e6e6"
| data-sort-value="1995"|1995{{snd}}1999
| style="border:4px ridge red; background:#000000;" rowspan=2 |[[File:Artist impression of the exoplanet 51 Pegasi b.jpg|112x112px]]
| [[Dimidium]] <br />''(51 Peg b)''
| data-sort-value="1.025"|''Unknown''
| style="text-align:center;" | –
| data-sort-value"0.4605"|0.46 {{±|0.06|0.01}}<ref name="Martins-2015" />
| First convincing exoplanet discovered orbiting a [[Main sequence|main-sequence]] star. Prototype [[hot Jupiter]].
|-
| data-sort-value="1994"|1995{{snd}}1995
| [[Dimidium]] <br />''(51 Peg b)''
| data-sort-value="1.02"|''Unknown''
| style="text-align:center;" | ←
| 0.46 {{±|0.06|0.01}}<ref name="Martins-2015" />
| First convincing exoplanet discovered orbiting a [[Main sequence|main-sequence]] star. Prototype [[hot Jupiter]].
|- style="background:#CEE0F2" 
| data-sort-value="1993"|(1993{{snd}}1995)
| style="border:4px ridge red; background:#000000;" |[[File:Artist's impression of pulsar planet B1620-26c.jpg|112x112px]]
| [[PSR B1620−26 b]]<br />''(PSR B1620-26 (AB) b,<br />"Methuselah")''
| data-sort-value="1.001"|''Unknown''
| style="text-align:center;" | →
| 2.5 ± 1''<ref name="Sigurdson">{{cite journal |author=Sigurdsson, S. |author2=Richer, H.B. |author3=Hansen, B.M. |author4=Stairs I.H. |author5=Thorsett, S.E. |date=2003 |title=A Young White Dwarf Companion to Pulsar B1620-26: Evidence for Early Planet Formation |journal=Science |volume=301 |issue=5630 |pages=193&ndash;196 |arxiv=astro-ph/0307339 |bibcode=2003Sci...301..193S |doi=10.1126/science.1086326 |pmid=12855802 |s2cid=39446560}}</ref>''
| 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,<ref name="Britt">{{cite web |author=Britt, Robert Roy |date=2003 |title=Primeval Planet: Oldest Known World Conjures Prospect of Ancient Life |url=http://thebookofbeginnings.com/sources/10/PrimevalPlanet.pdf |url-status=dead |archive-url=https://web.archive.org/web/20131219075138/http://thebookofbeginnings.com/sources/10/PrimevalPlanet.pdf |archive-date=2013-12-19 |access-date=2013-12-19 |work=Space.com}}</ref> hence the nickname, ''"Methuselah"''.<ref name="Sigurdson" /><ref name="STScI">{{cite web |title=Oldest Known Planet Identified |url=http://hubblesite.org/newscenter/newsdesk/archive/releases/2003/19/ |url-status=live |archive-url=https://web.archive.org/web/20080517012902/http://hubblesite.org/newscenter/newsdesk/archive/releases/2003/19/ |archive-date=2008-05-17 |access-date=2006-05-07 |work=HubbleSite}}</ref>
|-
| data-sort-value="1992"|1992{{snd}}1995
| style="border:4px ridge red; background:#000000; text-align:center;"|[[File:PSR B1257+12 B.jpg|112x112px]]
| [[PSR B1257+12 c|Poltergeist]]<br />''({{nowrap|PSR B1257+12 c}})''
| data-sort-value="0.089"|''Unknown''
| style="text-align:center;" | ←
| data-sort-value="0.0135"|0.013 53 ± 0.000 63<br />(4.3 ± 0.2 {{val|ul=Earth mass}})<ref name="nUpRl" />
| [[List of exoplanets discovered before 2000|First]] confirmed planet ever discovered outside the [[Solar System]] together with the less massive [[PSR B1257+12 b|Draugr]] ''(PSR B1257+12 b)'', one of three [[pulsar planet]]s known to be orbiting the [[pulsar]] [[PSR B1257+12|Lich]] ''(PSR B1257+12)''.<ref name="vYZFq" /><ref name="2LPxw" /> Unclear whether Lich planets are [[pulsar planet#Formation|survivors or formed in a second round of planet formation]] from the remnants of the [[supernova]].
|- style="background:#FFF8DC"
| data-sort-value="1989"|(1989{{snd}}1995)
|
| [[HD 114762 b|HD 114762 Ab]]<br />''("Latham's Planet")''
| data-sort-value="1.05"|''Unknown''
| style="text-align:center;" | *
| data-sort-value="11.069"|{{nowrap|11.069 ± 0.063,}}<ref name="wang" /><br />~63.2<ref name="Kane2012" />
| Discovered in 1989 by Latham to have a minimum mass of 11.069 ± 0.063 {{val|ul=Jupiter mass}} (at 90°) and a probable mass of approximately {{val|63.2|ul=Jupiter mass}} (at 10°),<ref name="Kane2012" /> making the former planet the first to be spotted,<ref name="first exoplanet">{{cite web |url=https://www.discovermagazine.com/the-sciences/the-fight-over-who-really-found-the-first-exoplanet |title=The fight over who really found the first exoplanet |website=Discover Magazine |date=April 22, 2019 |access-date=December 14, 2019}}</ref> and confirmed in 1991, it was thought to be the first discovered exoplanet until 2019 when it was confirmed to be a [[red dwarf|low-mass star]] with the mass of 147.0 {{±|39.3|42.0}} {{val|ul=Jupiter mass}},<ref name="2LAqC" /> making the [[PSR B1257+12 c|planet]] above the first confirmed exoplanet discovered ever.
|- style="background:#CEE0F2" 
| data-sort-value="1988"|(1988{{snd}}1992)
|style="border:4px ridge red; background:#000000; text-align:center;"|[[File:Gamma Cephei.png|112x112px]]
| [[Gamma Cephei Ab|Tadmor]]<br />''(Gamma Cephei Ab,<br />γ Cep Ab)''
| data-sort-value="0"|''Unknown''
| style="text-align:center;" | →
| 6.6 {{±|2.3|2.8}}<ref name="1cbau" />
|First evidence for exoplanet to receive later confirmation. First reported in 1988,<ref name="CikB8" /> making it arguably the first ''true'' exoplanet discovered, and independently in 1989,<ref name="LomZS" /> however, retracted in 1992<ref name="oyrqA" /> 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.<ref name="xAUtu" />
|- style="background:pink;" 
| data-sort-value="-600"|([[Jupiter#History|Antiquity]]{{snd}}1992, 1988 or 1995)
|style="border:4px ridge blue; background:#000000;"|[[File:Jupiter New Horizons.jpg|112x112px]]
| [[Jupiter]]
| 1<br />({{val|11.209|ul=Earth radius}})<ref name="Prša-2016" /><br />[[Jupiter radius|''(71 492 km)'']]
| style="text-align:center;" |{{number sign}}
| 1<br />({{val|317.827|ul=Earth mass}})<ref name="JPL Planets" /><br />''[[Jupiter mass|(1.898 125 × 10<sup>27</sup> kg)]]''
| [[Jupiter#Formation and migration|Oldest]], largest and most massive [[Solar System planets|planet]] in the [[Solar System]]<ref name=":1" /> Observations date back to 7th or 8th century BC. Using an early telescope the [[Galilean moons]] were discovered in 1610, the planet hosts [[Moons of Jupiter|95 known moons]].<br /><small>''Reported for reference.''</small>
|-class="sortbottom" 
| colspan="7" | For earlier entries, see [[Exoplanet#Early speculations|early speculations and discredited claims]].
|}

=== Notes ===
{{notelist}}

== 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]]

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<ref name="Britt">{{cite web |author=Britt, Robert Roy |date=2003 |title=Primeval Planet: Oldest Known World Conjures Prospect of Ancient Life |url=http://thebookofbeginnings.com/sources/10/PrimevalPlanet.pdf |url-status=dead |archive-url=https://web.archive.org/web/20131219075138/http://thebookofbeginnings.com/sources/10/PrimevalPlanet.pdf |archive-date=2013-12-19 |access-date=2013-12-19 |work=Space.com}}</ref>

<ref name="Sigurdson">{{cite journal |author=Sigurdsson, S. |author2=Richer, H.B. |author3=Hansen, B.M. |author4=Stairs I.H. |author5=Thorsett, S.E. |date=2003 |title=A Young White Dwarf Companion to Pulsar B1620-26: Evidence for Early Planet Formation |journal=Science |volume=301 |issue=5630 |pages=193&ndash;196 |arxiv=astro-ph/0307339 |bibcode=2003Sci...301..193S |doi=10.1126/science.1086326 |pmid=12855802 |s2cid=39446560}}</ref><ref name="STScI">{{cite web |title=Oldest Known Planet Identified |url=http://hubblesite.org/newscenter/newsdesk/archive/releases/2003/19/ |url-status=live |archive-url=https://web.archive.org/web/20080517012902/http://hubblesite.org/newscenter/newsdesk/archive/releases/2003/19/ |archive-date=2008-05-17 |access-date=2006-05-07 |work=HubbleSite}}</ref>

<ref name="8hZ77">{{Cite web |title=Observing Exoplanets: What Can We Really See? |url=https://science.nasa.gov/universe/exoplanets/observing-exoplanets-what-can-we-really-see/ |access-date=2024-08-16 |website=NASA Science|date=28 October 2019}}</ref>

<ref name="EKWXb">{{Cite web |title=Stanford scientists describe a gravity telescope that could image exoplanets |url=https://news.stanford.edu/stories/2022/05/gravity-telescope-image-exoplanets |access-date=2024-08-16 |website=Stanford University - Stanford Report}}</ref>

<ref name="UxcVg">{{Cite web |title=Just a few pixels would let astronomers map surface features like oceans and deserts on an exoplanet |url=https://phys.org/news/2022-04-pixels-astronomers-surface-features-oceans.html |access-date=2024-08-16 |website=Phys.org - (Universe Today)}}</ref><ref name="Ujyhy">{{cite web |author=Jerry Coffey |date=8 July 2008 |title=What is the Biggest Planet in the Solar System? |url=http://www.universetoday.com/15453/what-is-the-biggest-planet-in-the-solar-system/ |url-status=live |archive-url=https://web.archive.org/web/20141116084833/http://www.universetoday.com/15453/what-is-the-biggest-planet-in-the-solar-system/ |archive-date=16 November 2014 |access-date=7 November 2014 |publisher=Universe Today}}</ref>

<ref name="l60e2">{{Cite web |title=Planet KPNO-Tau 4 |url=https://exoplanet.eu/catalog/kpno_tau_4--9139/ |access-date=2024-08-15 |website=Encyclopaedia of exoplanetary systems / Exoplanet.eu}}</ref>

<ref name="WDjss">{{Cite journal |last1=Stolker |first1=Tomas |last2=Haffert |first2=Sebastiaan Y. |last3=Kesseli |first3=Aurora Y. |last4=van Holstein |first4=Rob G. |last5=Aoyama |first5=Yuhiko |last6=Brinchmann |first6=Jarle |last7=Cugno |first7=Gabriele |last8=Girard |first8=Julien H. |last9=Marleau |first9=Gabriel-Dominique |last10=Meyer |first10=Michael R. |last11=Milli |first11=Julien |last12=Quanz |first12=Sascha P. |last13=Snellen |first13=Ignas A. G. |last14=Todorov |first14=Kamen O. |date=2021-12-01 |title=Characterizing the Protolunar Disk of the Accreting Companion GQ Lupi B* |journal=The Astronomical Journal |volume=162 |issue=6 |page=286 |arxiv=2110.04307 |doi=10.3847/1538-3881/ac2c7f |bibcode=2021AJ....162..286S |s2cid=238582841 |issn=0004-6256 |doi-access=free}}</ref>

<ref name="LVyQ3">{{Cite journal |last1=Joergens |first1=V. |last2=Bonnefoy |first2=M. |last3=Liu |first3=Y. |last4=Bayo |first4=A. |last5=Wolf |first5=S. |last6=Chauvin |first6=G. |last7=Rojo |first7=P. |date=October 2013 |title=OTS 44: Disk and accretion at the planetary border |url=http://www.aanda.org/10.1051/0004-6361/201322432 |journal=Astronomy & Astrophysics |volume=558 |pages=L7 |arxiv=1310.1936 |bibcode=2013A&A...558L...7J |doi=10.1051/0004-6361/201322432 |issn=0004-6361}}</ref>

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<ref name="WRrrL">{{Cite journal |last1=Chakrabarty |first1=Aritra|last2=Sengupta|first2=Sujan|date=2019-07-01 |title=Precise Photometric Transit Follow-up Observations of Five Close-in Exoplanets: Update on Their Physical Properties |journal=The Astronomical Journal |volume=158 |issue=1 |page=39 |doi=10.3847/1538-3881/ab24dd |doi-access=free |arxiv=1905.11258 |bibcode=2019AJ....158...39C |issn=0004-6256}}</ref>

<ref name="EytJY">[http://www.ria.ru/science/20120206/558647431.html Российские астрономы впервые открыли луну возле экзопланеты] (in Russian) - "Studying of a curve of change of shine of WASP-12b has brought to the Russian astronomers unusual result: regular splashes were found out.<...> Though stains on a star surface also can cause similar changes of shine, observable splashes are very similar on duration, a profile and amplitude that testifies for benefit of exomoon existence."</ref>

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}}

{{Exoplanet}}

{{DEFAULTSORT:Largest exoplanets}}
[[Category:Lists of exoplanets|Largest]]
[[Category:Lists of superlatives in astronomy|Exoplanets, largest]]