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{{Short description|none}} {{Short description|none}}
] (Dagon), 25 light-years away, with its parent star ] blacked out, as pictured by ] in 2012.<ref>{{cite web| url=http://www.nasa.gov/mission_pages/hubble/science/rogue-fomalhaut.html| title=NASA's Hubble Reveals Rogue Planetary Orbit For Fomalhaut| date=2013-08-01| publisher=NASA| first1=J. D.| last1=Harrington| first2=Ray| last2=Villard| access-date=2015-09-18| url-status=live| archive-url=https://web.archive.org/web/20151106185243/http://www.nasa.gov/mission_pages/hubble/science/rogue-fomalhaut.html| archive-date=2015-11-06}}</ref> In 2020 this object was determined to be an expanding debris cloud from a collision of asteroids rather than a planet.<ref name="PNAS-20200420"/>]] ], 12 light-years away, with its parent star ] A blacked out, as pictured by ] in 2023.<ref>{{cite web |url=https://science.nasa.gov/missions/webb/nasas-webb-images-cold-exoplanet-12-light-years-away/ |title=NASA's Webb Images Cold Exoplanet 12 Light-Years Away |website=nasa.gov |publisher=NASA Webb Mission Team |access-date=Jul 24, 2024 |quote=}}</ref>]]
] ]


There are {{Extrasolar planet counts|planet_count}} known ]s, or planets outside the ] that orbit a star, as of {{Extrasolar planet counts|asof|mdy}}; only a small fraction of these are located in the vicinity of the Solar System.<ref name="Encyclopaedia"/> Within {{convert|10|pc|ly|lk=on|1|abbr=off}}, there are 104 exoplanets listed as confirmed by the ].{{efn|group=note|Listed values are primarily taken from '']'',<ref name=NASAed/> but other databases include a few additional exoplanet entries tagged as "Confirmed" that have yet to be compiled into the NASA archive. Such databases include: There are {{Extrasolar planet counts|planet_count}} known ]s, or planets outside the ] that orbit a star, as of {{Extrasolar planet counts|asof|mdy}}; only a small fraction of these are located in the vicinity of the Solar System.<ref name="Encyclopaedia"/> Within {{convert|10|pc|ly|lk=on|1|abbr=off}}, there are 106 exoplanets listed as confirmed by the ].{{efn|group=note|Listed values are primarily taken from '']'',<ref name=NASAed/> but other databases include a few additional exoplanet entries tagged as "Confirmed" that have yet to be compiled into the NASA archive. Such databases include:
:: {{cite web |url=http://exoplanet.eu/catalog/ | title = Exoplanet Catalog | website =] | at=}} :: {{cite encyclopedia |url=https://exoplanet.eu/catalog/ |encyclopedia=] | title = Exoplanet Catalog |date=1995 | at=}}
:: {{cite web |url=http://exoplanets.org/table/ |title=Exoplanets Data Explorer | website = Exoplanet Orbit Database | publisher = California Planet Survey | at=<small>Click the "+" button to visualize additional parameters</small>}} :: {{cite web |url=http://exoplanets.org/table/ |title=Exoplanets Data Explorer | website = Exoplanet Orbit Database | publisher = California Planet Survey | at=<small>Click the "+" button to visualize additional parameters</small>}}
:: {{cite web |url=http://www.openexoplanetcatalogue.com/systems/ |title=Open Exoplanet Catalogue |at=<small>Click the "Show options" to visualize additional parameters</small> |access-date=2015-02-14 |archive-url=https://web.archive.org/web/20170902215033/http://www.openexoplanetcatalogue.com/systems/ |archive-date=2017-09-02 |url-status=dead }}}}<ref name=NASAed/> Among the over 500 known stars and ]s within 10 parsecs,<ref name="Reylé2021"/>{{efn|group=note|For reference, the 100th closest known star system in April 2021 was ] (20.4 ly).<ref name="Reylé2021"/>}} around 60 have been confirmed to have planetary systems; 51 stars in this range are visible to the naked eye,{{efn|group=note|name=nakedeye|According to the ], an astronomical object is visible to the naked eye under "typical" dark-sky conditions in a rural area if it has an ] smaller than +6.5. To the unaided eye, the limiting magnitude is +7.6 to +8.0 under "excellent" dark-sky conditions (with effort).<ref name=nakedeye/>}}<ref name=autogenerated2/> eight of which have planetary systems. :: {{cite web |url=http://www.openexoplanetcatalogue.com/systems/ |title=Open Exoplanet Catalogue |at=<small>Click the "Show options" to visualize additional parameters</small> |access-date=2015-02-14 |archive-url=https://web.archive.org/web/20170902215033/http://www.openexoplanetcatalogue.com/systems/ |archive-date=2017-09-02 |url-status=dead }}}}<ref name=NASAed/> Among the over 500 known stars and ]s within 10 parsecs,<ref name="Reylé2021"/>{{efn|group=note|For reference, the 100th closest known star system in April 2021 was ] (20.4 ly).<ref name="Reylé2021"/>}} around 60 have been confirmed to have planetary systems; 51 stars in this range are visible to the naked eye,{{efn|group=note|name=nakedeye|According to the ], an astronomical object is visible to the naked eye under "typical" dark-sky conditions in a rural area if it has an ] smaller than +6.5. To the unaided eye, the limiting magnitude is +7.6 to +8.0 under "excellent" dark-sky conditions (with effort).<ref name=nakedeye/>}}<ref name=autogenerated2/> eight of which have planetary systems.


The first report of an exoplanet within this range was in 1998 for a planet orbiting around ] (15.3 light-years (ly) away), and the latest as of 2023 are two around ] (30.7 ly). The closest exoplanets are those found orbiting the star closest to the Solar System, which is ] 4.25 light-years away. The first confirmed exoplanet discovered in the Proxima Centauri system was ], in 2016. ] (21.6 ly) has six exoplanets, the highest number discovered for any star within this range. The first report of an exoplanet within this range was in 1998 for a planet orbiting around ] (15.3 light-years (ly) away), and the latest as of 2024 is one around ] A (11.5 ly). The closest exoplanets are those found orbiting the star closest to the Solar System, which is ] 4.25 light-years away. The first confirmed exoplanet discovered in the Proxima Centauri system was ], in 2016. ] (21.6 ly) has six exoplanets, the highest number discovered for any star within this range.


Most known nearby exoplanets orbit close to their stars. A majority are significantly larger than Earth, but a few have similar masses, including planets around ], ], and Proxima Centauri which may be less massive than Earth. Several confirmed exoplanets are hypothesized to be ], with Proxima Centauri b and ] (15.8 ly) considered among the most likely candidates.<ref name=PHL/> The ] has assigned proper names to some known extrasolar bodies, including nearby exoplanets, through the ] project. Planets named in the 2015 event include the planets around ] (10.5 ly) and ],{{efn|group=note|The star ] was named ''Ran'' (after ], the Norse goddess of the sea), and the planet ] was named ''AEgir'' (after ], Rán's husband),<ref>{{cite web |url=http://nameexoworlds.iau.org/systems/105 |title=epsilon Eridani |website=NameExoWorlds |publisher=International Astronomical Union |access-date=2018-05-14 |url-status=dead |archive-url=https://web.archive.org/web/20180215023352/http://nameexoworlds.iau.org/systems/105 |archive-date=2018-02-15 }}</ref> while the planet ] was named ''Dagon'' (after ], an ancient Syrian “fish god”<ref>{{cite web |url=http://nameexoworlds.iau.org/systems/103 |title=Fomalhaut (alpha Piscis Austrini) |website=Nameexoworlds |publisher=International Astronomical Union |access-date=2018-05-14 |url-status=dead |archive-url=https://web.archive.org/web/20170430100341/http://nameexoworlds.iau.org/systems/103 |archive-date=2017-04-30 }}</ref>).<ref name=IAUpoll/>}}<ref name=IAUpoll/> while planets named in the 2022 event include those around ], ], and ].<ref name="NEW2022"/> Most known nearby exoplanets orbit close to their stars. A majority are significantly larger than Earth, but a few have similar masses, including planets around ], ], Proxima Centauri, and ] which may be less massive than Earth. Several confirmed exoplanets are hypothesized to be ], with Proxima Centauri b and ] (15.8 ly) considered among the most likely candidates.<ref name=PHL/> The ] has assigned proper names to some known extrasolar bodies, including nearby exoplanets, through the ] project. Planets named in the 2015 event include the planets around ] (10.5 ly) and ],{{efn|group=note|The star ] was named ''Ran'' (after ], the Norse goddess of the sea), and the planet ] was named ''AEgir'' (after ], Rán's husband),<ref>{{cite web |url=http://nameexoworlds.iau.org/systems/105 |title=epsilon Eridani |website=NameExoWorlds |publisher=International Astronomical Union |access-date=2018-05-14 |url-status=dead |archive-url=https://web.archive.org/web/20180215023352/http://nameexoworlds.iau.org/systems/105 |archive-date=2018-02-15 }}</ref> while the planet ] was named ''Dagon'' (after ], an ancient Syrian “fish god”<ref>{{cite web |url=http://nameexoworlds.iau.org/systems/103 |title=Fomalhaut (alpha Piscis Austrini) |website=Nameexoworlds |publisher=International Astronomical Union |access-date=2018-05-14 |url-status=dead |archive-url=https://web.archive.org/web/20170430100341/http://nameexoworlds.iau.org/systems/103 |archive-date=2017-04-30 }}</ref>).<ref name=IAUpoll/>}}<ref name=IAUpoll/> while planets named in the 2022 event include those around ], ], and ].<ref name="NEW2022"/>


==Exoplanets within 10 parsecs== ==Exoplanets within 10 parsecs==
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|align=left|Exoplanets believed to be ]<ref name=PHL/> |align=left|Exoplanets believed to be ]<ref name=PHL/>
|} |}
{{sticky header}}
{| class="wikitable sortable" style="text-align:center;"
{| class="wikitable sortable sticky-header-multi" style="text-align:center;"
|+ style="background:white" | Confirmed exoplanets<ref name=NASAed/> |+ style="background:white" | Confirmed exoplanets<ref name=NASAed/>
|- |-
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| ] || {{sort|0043.9000|≥43.9}} || — || 1.845 || {{sort|2938|2,940}} || 0.04 || — || ] || 2019 || <ref name="Barnes2019"/> | ] || {{sort|0043.9000|≥43.9}} || — || 1.845 || {{sort|2938|2,940}} || 0.04 || — || ] || 2019 || <ref name="Barnes2019"/>
--> -->
|-
! scope="row" style="background:#F8F9FA; font-weight:normal; padding-right:0.4em;" | ]
|5.9629
|9.51
|0.162
|b
|≥0.37
|—
|0.0229
|3.153
|0.16
|—
|]
|2024
|<ref>{{Cite web |last=ESO |title=Scientists discover planet orbiting closest single star to our sun |url=https://phys.org/news/2024-09-scientists-planet-orbiting-closest-star.html#google_vignette |access-date=2024-10-05 |website=phys.org |language=en}}</ref><ref>{{Cite journal |last=Hernández |first=J. I. González |last2=Mascareño |first2=A. Suárez |last3=Silva |first3=A. M. |last4=Stefanov |first4=A. K. |last5=Faria |first5=J. P. |last6=Tabernero |first6=H. M. |last7=Sozzetti |first7=A. |last8=Rebolo |first8=R. |last9=Pepe |first9=F. |last10=Santos |first10=N. C. |last11=Cristiani |first11=S. |last12=Lovis |first12=C. |last13=Dumusque |first13=X. |last14=Figueira |first14=P. |last15=Lillo-Box |first15=J. |date=2024-10-01 |title=A sub-Earth-mass planet orbiting Barnard’s star |url=https://www.aanda.org/articles/aa/full_html/2024/10/aa51311-24/aa51311-24.html |journal=Astronomy & Astrophysics |language=en |volume=690 |pages=A79 |doi=10.1051/0004-6361/202451311 |issn=0004-6361|arxiv=2410.00569 }}</ref>
|- style="background:#ffffb0;" |- style="background:#ffffb0;"
! scope="row" rowspan="2" style="background:#ffffb0; font-weight:normal; padding-right:0.4em;" | ]<sup>#</sup> ! scope="row" rowspan="2" style="background:#ffffb0; font-weight:normal; padding-right:0.4em;" | ]<sup>#</sup>
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| ] || {{sort|0013.1000|≥13.1}} || — || 0.428 || {{sort|0192.4|192}} || 0.03 || — || ] || 2019 | ] || {{sort|0013.1000|≥13.1}} || — || 0.428 || {{sort|0192.4|192}} || 0.03 || — || ] || 2019
--> -->
|-
! scope="row" style="background:#F8F9FA; font-weight:normal; padding-right:0.4em;" | ] A
|11.491
|8.94
|0.330
|]
|≥2.78
|—
|0.068
|11.2201
|0.0
|—
|]
|2024
|<ref>{{Citation |last=Cortes-Zuleta |first=P. |title=Gl 725A b: a potential super-Earth detected with SOPHIE and SPIRou in an M dwarf binary system at 3.5 pc |date=2024-11-14 |url=https://arxiv.org/abs/2411.09506 |access-date=2024-11-27 |doi=10.48550/arXiv.2411.09506 |last2=Boisse |first2=I. |last3=Ould-Elhkim |first3=M. |last4=Wilson |first4=T. G. |last5=Larue |first5=P. |last6=Carmona |first6=A. |last7=Delfosse |first7=X. |last8=Donati |first8=J.-F. |last9=Forveille |first9=T.}}</ref>
|- style="background:#ffffb0;" |- style="background:#ffffb0;"
! scope="row" rowspan="2" style="background:#FFFFB0; font-weight:normal; padding-right:0.4em;" | ] A<sup>#</sup> ! scope="row" rowspan="2" style="background:#FFFFB0; font-weight:normal; padding-right:0.4em;" | ] A<sup>#</sup>
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| scope="row" style="background:#F8F9FA; font-weight:normal; padding-right:0.4em;" | ] A | scope="row" style="background:#F8F9FA; font-weight:normal; padding-right:0.4em;" | ] A
| 11.867 || {{sort|483|4.83}} || 0.762 | 11.867 || {{sort|483|4.83}} || 0.762
| ] || 941 || — || 11.08 || {{sort|15676.48|15,700}} || 0.42 || 98.7 || ] || 2018 | ] || 2005 || — || 28.4 || {{sort|63400|63,400}} || 0.40 || 103.7 || ] || 2018
| <ref name="Feng2019"/><ref name="Feng2023"/> | nearest exoplanet directly imaged<ref name="Feng2019"/><ref name="Matthews2024"/>


|- style="background:#ffffb0;" |- style="background:#ffffb0;"
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| rowspan = "4" | 11.912 || rowspan = "4" | {{sort|0350|3.50}} || rowspan = "4" | 0.78 | rowspan = "4" | 11.912 || rowspan = "4" | {{sort|0350|3.50}} || rowspan = "4" | 0.78
| {{sort|g|]}} || {{sort|0001.7500|≥1.75}}|| — || 0.133 || {{sort|0020|20.0}} || 0.06 || ''~35?'' || ] || 2017 | {{sort|g|]}} || {{sort|0001.7500|≥1.75}}|| — || 0.133 || {{sort|0020|20.0}} || 0.06 || ''~35?'' || ] || 2017
| rowspan = "4" | 4 candidates<br><ref>{{cite web|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=tau+Cet |title=tau Cet |website=NASA Exoplanet Science Institute|publisher=California Institute of Technology|access-date=2018-03-22}}</ref><ref>{{cite web |url=http://www.openexoplanetcatalogue.com/system.html?id=tau%20Ceti%20b |title=tau Ceti |publisher=Open Exoplanet Catalogue |access-date=2014-05-17 |url-status=live |archive-url=https://web.archive.org/web/20140314114906/http://www.openexoplanetcatalogue.com/system.html?id=tau%20Ceti%20b |archive-date=2014-03-14 }}</ref><ref name=PHL/><ref>{{cite web|url=http://exoplanet.eu/catalog/tau_cet_b/|title=tau Cet b|website=The Extrasolar Planet Encyclopaedia|publisher=Exoplanet.eu|access-date=2018-03-22|url-status=live|archive-url=https://web.archive.org/web/20171107234328/http://exoplanet.eu/catalog/tau_cet_b/|archive-date=2017-11-07}}</ref><ref>{{cite web|url=http://exoplanet.eu/catalog/tau_cet_c/|title=tau Cet c|website=The Extrasolar Planet Encyclopaedia|publisher=Exoplanet.eu|access-date=2018-03-22|url-status=live|archive-url=https://web.archive.org/web/20171201042109/http://exoplanet.eu/catalog/tau_cet_c/|archive-date=2017-12-01}}</ref><ref>{{cite web |url=http://exoplanet.eu/catalog/tau_cet_d/ |title=tau Cet d |website=The Extrasolar Planet Encyclopaedia |publisher=Exoplanet.eu |access-date=2018-03-22 |url-status=live |archive-url=https://web.archive.org/web/20171201042106/http://exoplanet.eu/catalog/tau_cet_d/ |archive-date=2017-12-01 }}</ref> | rowspan = "4" | 4 disputed candidates<br><ref>{{cite web|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=tau+Cet |title=tau Cet |website=NASA Exoplanet Science Institute|publisher=California Institute of Technology|access-date=2018-03-22}}</ref><ref>{{cite web |url=http://www.openexoplanetcatalogue.com/system.html?id=tau%20Ceti%20b |title=tau Ceti |publisher=Open Exoplanet Catalogue |access-date=2014-05-17 |url-status=live |archive-url=https://web.archive.org/web/20140314114906/http://www.openexoplanetcatalogue.com/system.html?id=tau%20Ceti%20b |archive-date=2014-03-14 }}</ref><ref name=PHL/><ref>{{cite encyclopedia|url=https://exoplanet.eu/catalog/tau_cet_b--1234/|title=tau Cet b|access-date=2018-03-22|url-status=live|archive-url=https://web.archive.org/web/20171107234328/http://exoplanet.eu/catalog/tau_cet_b/|encyclopedia=]|archive-date=2017-11-07}}</ref><ref>{{cite encyclopedia|url=https://exoplanet.eu/catalog/tau_cet_c--1235/|title=tau Cet c|access-date=2018-03-22|url-status=live|archive-url=https://web.archive.org/web/20171201042109/http://exoplanet.eu/catalog/tau_cet_c/|encyclopedia=]|archive-date=2017-12-01}}</ref><ref>{{cite encyclopedia |url=https://exoplanet.eu/catalog/tau_cet_d--1236/ |title=tau Cet d |access-date=2018-03-22 |url-status=live |archive-url=https://web.archive.org/web/20171201042106/http://exoplanet.eu/catalog/tau_cet_d/ |encyclopedia=] |archive-date=2017-12-01 }}</ref>
|- style="background:#ffffb0;" |- style="background:#ffffb0;"
| {{sort|h|]}} || {{sort|0001.8300|≥1.8}} || — || 0.243 || {{sort|0049|49.4}} || 0.23 || ''~35?'' || ] || 2017 | {{sort|h|]}} || {{sort|0001.8300|≥1.8}} || — || 0.243 || {{sort|0049|49.4}} || 0.23 || ''~35?'' || ] || 2017
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|- style="background:#ffffb0;" |- style="background:#ffffb0;"
! scope="row" rowspan="2" style="background:#FFFFB0; font-weight:normal; padding-right:0.4em;" | ]<sup>#</sup> ! scope="row" rowspan="3" style="background:#FFFFB0; font-weight:normal; padding-right:0.4em;" | ]<sup>#</sup>
| rowspan="2" |12.497 ||rowspan="2" | {{sort|1540|15.40}} ||rowspan="2" | 0.08 | rowspan="3" |12.497 ||rowspan="3" | {{sort|1540|15.40}} ||rowspan="3" | 0.08
| style="background:#BCD4E6;" | ]<sup>↑</sup> || style="background:#BCD4E6;" | {{sort|0001.0500|≥1.05}} || style="background:#BCD4E6;" | — || style="background:#BCD4E6;" | 0.0252 || style="background:#BCD4E6;" | 4.910 || style="background:#BCD4E6;" | 0 || style="background:#BCD4E6;" | — ||style="background:#BCD4E6;" | ] || style="background:#BCD4E6;" | 2019 | style="background:#BCD4E6;" | ]<sup>↑</sup> || style="background:#BCD4E6;" | {{sort|0001.1600|≥1.16}} || style="background:#BCD4E6;" | — || style="background:#BCD4E6;" | 0.0259 || style="background:#BCD4E6;" | 4.906 || style="background:#BCD4E6;" | 0.03 || style="background:#BCD4E6;" | — ||style="background:#BCD4E6;" | ] || style="background:#BCD4E6;" | 2019
| rowspan="2" |<ref name="CARMENES"/> | rowspan="3" |<ref name="CARMENES"/><ref name="Dreizler2024"/>
|- style="background:#BCD4E6;" |- style="background:#BCD4E6;"
| ]<sup>↑</sup> || {{sort|0001.1100|≥1.11}} || — || 0.0443 || 11.41 || 0 || — || ] || 2019 | ]<sup>↑</sup> || {{sort|0001.0500|≥1.05}} || — || 0.0455 || 11.42 || 0.04 || — || ] || 2019
|- style="background:#ffffb0;"
| ] || {{sort|0000.8200|≥0.82}} || — || 0.0791 || 26.13 || 0.07 || — || ] || 2024


|- style="background:#ffffb0;" |- style="background:#ffffb0;"
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| rowspan = "2"| 17.531 || rowspan = "2"| {{sort|1220|12.2}} || rowspan = "2"| 0.164 | rowspan = "2"| 17.531 || rowspan = "2"| {{sort|1220|12.2}} || rowspan = "2"| 0.164
| ] || {{sort|0002.0200|≥2.0}} || — || 0.0328 || {{sort|0005.36|5.36}}|| {{sort|0.23|0.2}} || — || ] || 2017 | ] || {{sort|0002.0200|≥2.0}} || — || 0.0328 || {{sort|0005.36|5.36}}|| {{sort|0.23|0.2}} || — || ] || 2017
| rowspan = "2"| <ref name="Astudillo-Defru2017"/>
| rowspan = "2"| <ref>{{cite web|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=GJ+3323 |title=GJ 3323 |website=NASA Exoplanet Science Institute|publisher=California Institute of Technology|access-date=2018-03-22}}</ref>
|- style="background:#ffffb0;" |- style="background:#ffffb0;"
| ] || {{sort|0002.3100|≥2.3}} || — || 0.126 || {{sort|0040.5|40.5}} || {{sort|0.17|0.2}} || — || ] || 2017 | ] || {{sort|0002.3100|≥2.3}} || — || 0.126 || {{sort|0040.5|40.5}} || {{sort|0.17|0.2}} || — || ] || 2017
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| rowspan="2"| 18.791 ||rowspan="2"| {{sort|0814|8.14}} ||rowspan="2"|0.58 | rowspan="2"| 18.791 ||rowspan="2"| {{sort|0814|8.14}} ||rowspan="2"|0.58
| style="background:#BCD4E6;" | ]<sup>↑</sup> || style="background:#BCD4E6;" | {{sort|0007.3000|≥7.3}} || style="background:#BCD4E6;" | — || style="background:#BCD4E6;" | 0.339 || style="background:#BCD4E6;" | {{sort|0122.0|122}} || style="background:#BCD4E6;" | 0.19 || style="background:#BCD4E6;" | — ||style="background:#BCD4E6;" | ] || style="background:#BCD4E6;" | 2020 | style="background:#BCD4E6;" | ]<sup>↑</sup> || style="background:#BCD4E6;" | {{sort|0007.3000|≥7.3}} || style="background:#BCD4E6;" | — || style="background:#BCD4E6;" | 0.339 || style="background:#BCD4E6;" | {{sort|0122.0|122}} || style="background:#BCD4E6;" | 0.19 || style="background:#BCD4E6;" | — ||style="background:#BCD4E6;" | ] || style="background:#BCD4E6;" | 2020
| rowspan="2"| Ab not confirmed until 2020.<ref name="Feng2020"/> | rowspan="2"| Ab not confirmed until 2020<ref name="Feng2020"/>
|- style="background:#ffffb0;" |- style="background:#ffffb0;"
| ] || {{sort|0008.5000|≥8.5}} || — || 0.898 || {{sort|0526.1|526}} || 0.10 || — || ] || 2014 | ] || {{sort|0008.5000|≥8.5}} || — || 0.898 || {{sort|0526.1|526}} || 0.10 || — || ] || 2014
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! scope="row" style="background:#F8F9FA; font-weight:normal; padding-right:0.4em;"| ] A ! scope="row" style="background:#F8F9FA; font-weight:normal; padding-right:0.4em;"| ] A
| 19.292 || {{sort|0913|9.13}} ||0.46 | 19.292 || {{sort|0913|9.13}} ||0.46
| ] || {{sort|0013.6000|≥13.6}} || — || 0.338 || {{sort|0106.2|106}} || 0.03 || — || ] || 2018 | ] || {{sort|0012.2140|≥12.2}} || — || 0.343 || {{sort|0105.9|106}} || 0.10 || — || ] || 2018
| <ref>{{cite journal |doi=10.1051/0004-6361/201833354 |last1=Kaminski |first1=Adrian |last2=Trifonov |first2=Trifon |last3=Caballero |first3=José A. |last4=Quirrenbach |first4=Andreas |last5=Ribas |first5=Ignasi |last6=Reiners |first6=Ansgar |last7=Amado |first7=Pedro J. |last8=Zechmeister |first8=Mathias |last9=Dreizler |first9=Stefan |last10=Perger |first10=Manuel |last11=Tal-Or |first11=Lev |last12=Bonfils |first12=Xavier |last13=Mayor |first13=Michel |last14=Astudillo-Defru |first14=Nicola |last15=Bauer |first15=Florian F. |last16=Béjar |first16=Victor J. S. |last17=Cifuentes |first17=Carlos |last18=Colomé |first18=Josep |last19=Cortés-Contreras |first19=Miriam |last20=Delfosse |first20=Xavier |last21=Díez-Alonso |first21=Enrique |last22=Forveille |first22=Thierry |last23=Guenther |first23=Eike W. |last24=Hatzes |first24=Artie P. |last25=Henning |first25=Thomas K. |last26=Jeffers |first26=Sandra V. |last27=Kürster |first27=Martin |last28=Lafarga |first28=Marina |last29=Luque |first29=Rafael |last30=Mandel |first30=Holger |last31=Montes |first31=David |last32=Morales |first32=Juan Carlos |last33=Passegger |first33=Vera Maria |last34=Pedraz |first34=Sandos |last35=Reffert |first35=Sabine |last36=Sadegi |first36=Sepideh |last37=Schweitzer |first37=Andreas |last38=Seifert |first38=Walter |last39=Stahl |first39=Otmar |last40=Udry |first40=Stéphane |title=The CARMENES search for exoplanets around M dwarfs. A Neptune-mass planet traversing the habitable zone around HD 180617 |journal=Astronomy & Astrophysics |volume=618 |pages=A115 |date=3 August 2018 |arxiv=1808.01183 |bibcode=2018A&A...618A.115K |s2cid=118980171 }}</ref><ref name="Barnes2019" /> | <ref>{{cite journal |doi=10.1051/0004-6361/201833354 |last1=Kaminski |first1=Adrian |last2=Trifonov |first2=Trifon |last3=Caballero |first3=José A. |last4=Quirrenbach |first4=Andreas |last5=Ribas |first5=Ignasi |last6=Reiners |first6=Ansgar |last7=Amado |first7=Pedro J. |last8=Zechmeister |first8=Mathias |last9=Dreizler |first9=Stefan |last10=Perger |first10=Manuel |last11=Tal-Or |first11=Lev |last12=Bonfils |first12=Xavier |last13=Mayor |first13=Michel |last14=Astudillo-Defru |first14=Nicola |last15=Bauer |first15=Florian F. |last16=Béjar |first16=Victor J. S. |last17=Cifuentes |first17=Carlos |last18=Colomé |first18=Josep |last19=Cortés-Contreras |first19=Miriam |last20=Delfosse |first20=Xavier |last21=Díez-Alonso |first21=Enrique |last22=Forveille |first22=Thierry |last23=Guenther |first23=Eike W. |last24=Hatzes |first24=Artie P. |last25=Henning |first25=Thomas K. |last26=Jeffers |first26=Sandra V. |last27=Kürster |first27=Martin |last28=Lafarga |first28=Marina |last29=Luque |first29=Rafael |last30=Mandel |first30=Holger |last31=Montes |first31=David |last32=Morales |first32=Juan Carlos |last33=Passegger |first33=Vera Maria |last34=Pedraz |first34=Sandos |last35=Reffert |first35=Sabine |last36=Sadegi |first36=Sepideh |last37=Schweitzer |first37=Andreas |last38=Seifert |first38=Walter |last39=Stahl |first39=Otmar |last40=Udry |first40=Stéphane |title=The CARMENES search for exoplanets around M dwarfs. A Neptune-mass planet traversing the habitable zone around HD 180617 |journal=Astronomy & Astrophysics |volume=618 |pages=A115 |date=3 August 2018 |arxiv=1808.01183 |bibcode=2018A&A...618A.115K |s2cid=118980171 }}</ref><ref name="Burt2021"/>
<!-- <!--
|- style="background:#ffffb0;" |- style="background:#ffffb0;"
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--> -->
|- style="background:#ffffb0;"<!---HD 20794---> |- style="background:#ffffb0;"<!---HD 20794--->
! scope="row" rowspan="4" style="background:#FFFFB0; font-weight:normal; padding-right:0.4em;" |]<sup>#</sup> ! scope="row" rowspan="2" style="background:#FFFFB0; font-weight:normal; padding-right:0.4em;" |]<sup>#</sup>
| rowspan = "4"|19.704 || rowspan = "4"|{{sort|0426|4.26}} ||rowspan = "4"|0.85 | rowspan = "2"|19.704 || rowspan = "2"|{{sort|0426|4.26}} ||rowspan = "2"|0.85
| ] || {{sort|0002.7000|≥2.7}} || — || 0.121 || {{sort|0018|18.3}} || {{sort|0|~0}} || — || ] || 2011 | ] || {{sort|0002.0000|≥2.0}} || — || 0.13 || {{sort|0018.32|18.3}} || 0.09 || — || ] || 2011
| rowspan = "4"|2 candidates<br><ref>{{cite web|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=HD+20794 |title=HD 20794 |website=NASA Exoplanet Science Institute|publisher=California Institute of Technology|access-date=2018-03-22}}</ref><ref>{{cite web |url=http://exoplanet.eu/catalog/hd_20794_f/ |website=The Extrasolar Planet Encyclopaedia |title=HD 20794 f |publisher=Exoplanet.eu |access-date=2018-03-22 |url-status=live |archive-url=https://web.archive.org/web/20180320170746/http://exoplanet.eu/catalog/hd_20794_f/ |archive-date=2018-03-20 }}</ref><ref>{{cite web |url=http://exoplanet.eu/catalog/hd_20794_g/ |website=The Extrasolar Planet Encyclopaedia |title=HD 20794 g |publisher=Exoplanet.eu |access-date=2018-03-22 |url-status=live |archive-url=https://web.archive.org/web/20180320170252/http://exoplanet.eu/catalog/hd_20794_g/ |archive-date=2018-03-20 }}</ref> | rowspan = "2"|5 disputed candidates<br><ref>{{cite web|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=HD+20794 |title=HD 20794 |website=NASA Exoplanet Science Institute|publisher=California Institute of Technology|access-date=2018-03-22}}</ref><ref>{{cite encyclopedia |url=https://exoplanet.eu/catalog/hd_20794_f--6565/ |title=HD 20794 f |access-date=2018-03-22 |url-status=live |archive-url=https://web.archive.org/web/20180320170746/http://exoplanet.eu/catalog/hd_20794_f/ |encyclopedia=] |archive-date=2018-03-20 }}</ref><ref>{{cite encyclopedia |url=https://exoplanet.eu/catalog/hd_20794_g--6566/ |title=HD 20794 g |access-date=2018-03-22 |url-status=live |archive-url=https://web.archive.org/web/20180320170252/http://exoplanet.eu/catalog/hd_20794_g/ |encyclopedia=] |archive-date=2018-03-20 }}</ref><ref name="Cretignier2023"/>
|- style="background:#ffffb0;" |- style="background:#ffffb0;"
| ] || {{sort|0002.4000|≥2.4}} || — || 0.204 || {{sort|0040|40.1}} || {{sort|0|~0}} || — || ] || 2011 | ] || {{sort|0004.7000|≥4.7}} || — || 0.37 || {{sort|0089.58|89.6}} || 0.13 || — || ] || 2011
|- style="background:#ffffb0;"
| ] || {{sort|0004.8000|≥4.8}} || — || 0.350 || {{sort|0090.3|90}} || {{sort|0|~0}} || — || ] || 2011
|- style="background:#ffffb0;"
| ] || {{sort|0004.7700|≥4.8}} || — || 0.509 || {{sort|0147|147}} || {{sort|0.29| 0.29}} || — || ] || 2017


<!----------- 20 ly ------> <!----------- 20 ly ------>
Line 287: Line 316:
| ] || {{sort|0009.4000|≥9.4}} || — || 0.059 || {{sort|0006.6592|6.66}} || 0.05 || — || ] || 2019 | ] || {{sort|0009.4000|≥9.4}} || — || 0.059 || {{sort|0006.6592|6.66}} || 0.05 || — || ] || 2019
| <ref name="Barnes2019"/> | <ref name="Barnes2019"/>
-->

|- |-
! scope="row" style="background:#F8F9FA; font-weight:normal; padding-right:0.4em;" | ] ! scope="row" style="background:#F8F9FA; font-weight:normal; padding-right:0.4em;" | ]
| 20.395 || {{sort|1131.7|11.32}} || 0.29 | 20.395 || {{sort|1131.7|11.32}} || 0.29
| ] || {{sort|0030.1000|≥30.1}} || — || 0.727 || {{sort|0449.6|450}} || 0.04 || — || ] || 2019 | ] || {{sort|0005.4600|≥5.5}} || — || 0.142 || {{sort|0036.116|36.1}} || 0.08 || — || ] || 2023
| <ref name="Barnes2019"/> | 1 candidate<ref name="González-Álvarez2023"/>

-->
|- |-
! scope="row" style="background:#F8F9FA; font-weight:normal; padding-right:0.4em;" | ] A ! scope="row" style="background:#F8F9FA; font-weight:normal; padding-right:0.4em;" | ] A
| 20.400 || {{sort|1038|10.38}} || 0.436 | 20.400 || {{sort|1038|10.38}} || 0.436
| ] || {{sort|0718|718}} || — || 0.643 || {{sort|0284.39|284}} || 0.35 || 69.2 || ] || 2022 | ] || {{sort|0718|718}} || — || 0.643 || {{sort|0284.39|284}} || 0.35 || 69.2 || <small>]</small> || 2022
| <ref name="Curiel2022"/> | <ref name="Curiel2022"/>


|- style="background:#ffffb0;" |- style="background:#ffffb0;"
! scope="row" rowspan="3" style="background:#FFFFB0; font-weight:normal; padding-right:0.4em;" |]<sup>#</sup> ! scope="row" rowspan="3" style="background:#FFFFB0; font-weight:normal; padding-right:0.4em;" |]<sup>#</sup>
| rowspan = "3"|20.549 ||rowspan = "3"|{{sort|1055|10.5}} || rowspan = "3"|0.31 | rowspan = "3"|20.549 ||rowspan = "3"|{{sort|1055|10.5}} || rowspan = "3"|0.295
| ] || {{sort|0001.7000|≥1.7}} || — || 0.0282 || {{sort|00032|3.15}} || 0.0 || ''~45?'' || ] || 2009 | ] || {{sort|0002.4800|2.5}} || — || 0.0280 || {{sort|0003.1481|3.15}} || 0.01 || 47 || ] || 2009
|rowspan = "3"| 3 refuted candidates and a ]<ref name="vonStauffenberg2024"/>
|rowspan = "3"| 3 refuted candidates and a ]<br><ref>{{cite web|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=GJ+581 |title=GJ 581 |website=NASA Exoplanet Science Institute|publisher=California Institute of Technology |access-date=2018-03-22}}</ref><ref>{{cite web |url=http://exoplanet.eu/catalog/gj_581_d/ |website=The Extrasolar Planet Encyclopaedia |title=GJ 581 d |publisher=Exoplanet.eu |access-date=2018-03-22 |url-status=live |archive-url=https://web.archive.org/web/20171201042658/http://exoplanet.eu/catalog/gj_581_d/ |archive-date=2017-12-01 }}</ref><ref>{{cite web |url=http://exoplanet.eu/catalog/gj_581_f/ |website=The Extrasolar Planet Encyclopaedia |title=GJ 581 f |publisher=Exoplanet.eu |access-date=2018-03-22 |url-status=live |archive-url=https://web.archive.org/web/20180320230447/http://exoplanet.eu/catalog/gj_581_f/ |archive-date=2018-03-20 }}</ref><ref>{{cite web |url=http://exoplanet.eu/catalog/gj_581_g/ |website=The Extrasolar Planet Encyclopaedia |title=GJ 581 g |publisher=Exoplanet.eu |access-date=2018-03-22 |url-status=live |archive-url=https://web.archive.org/web/20180324064754/http://exoplanet.eu/catalog/gj_581_g/ |archive-date=2018-03-24 }}</ref>
|- style="background:#ffffb0;" |- style="background:#ffffb0;"
| ] || {{sort|0015.8000|≥16}} || — || 0.0406 || {{sort|00054|5.37}} || 0.0 || ''~45?'' || ] || 2005 | ] || {{sort|0020.5000|20.5}} || — || 0.0399 || {{sort|0005.3686|5.37}} || 0.03 || 47 || ] || 2005
|- style="background:#ffffb0;" |- style="background:#ffffb0;"
| ] || {{sort|0005.5000|≥5.5}} || — || 0.072 || {{sort|0013|12.9}} || 0.0 || ''~45?'' || ] || 2007 | ] || {{sort|0006.8100|6.8}} || — || 0.0718 || {{sort|0012.9211|12.9}} || 0.03 || 47 || ] || 2007


|- |-
Line 342: Line 371:
| rowspan="2"| 22.387 || rowspan="2"| {{sort|1052.9|10.53}} ||rowspan="2"| 0.26 | rowspan="2"| 22.387 || rowspan="2"| {{sort|1052.9|10.53}} ||rowspan="2"| 0.26
| ] || {{sort|0001.5400|1.54}} || 1.15 || 0.0266 || {{sort|0003.12390|3.12}} || <0.22 || 87.43 || ] || 2021 | ] || {{sort|0001.5400|1.54}} || 1.15 || 0.0266 || {{sort|0003.12390|3.12}} || <0.22 || 87.43 || ] || 2021
| rowspan="2"| <ref name="Almenara2019"/><ref name="Winters2021"/> | rowspan="2"| 1 candidate<ref name="Almenara2019"/><ref name="Winters2021"/><ref name="Lavie2023"/>
|- style="background:#ffffb0;" |- style="background:#ffffb0;"
| ] || {{sort|0002.8700|2.87}} || 1.30 || 0.0381 || {{sort|0005.35877|5.36}} || <0.11 || 89.68 || ] || 2019 | ] || {{sort|0002.8700|2.87}} || 1.30 || 0.0381 || {{sort|0005.35877|5.36}} || <0.11 || 89.68 || ] || 2019
Line 362: Line 391:
| rowspan = "2"|23.623 || rowspan = "2"|{{sort|1022|10.2}} || rowspan = "2"|0.33 | rowspan = "2"|23.623 || rowspan = "2"|{{sort|1022|10.2}} || rowspan = "2"|0.33
| {{sort|b3|]}} || {{sort|0005.4000|≥5.4}} || — || 0.049 || {{sort|00072|7.20}} || 0.13 || ''~52?'' || ] || 2009 | {{sort|b3|]}} || {{sort|0005.4000|≥5.4}} || — || 0.049 || {{sort|00072|7.20}} || 0.13 || ''~52?'' || ] || 2009
| rowspan = "2"|5 dubious candidates<br><ref>{{cite web|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=GJ+667+C |title=GJ 667 C |website=NASA Exoplanet Science Institute|publisher=California Institute of Technology|access-date=2018-03-22}}</ref><ref name=PHL/><ref>{{cite web|url=http://exoplanet.eu/catalog/gj_667_c_d/|title=GJ 667 C d|website=The Extrasolar Planet Encyclopaedia|publisher=Exoplanet.eu|access-date=2018-03-22|url-status=live|archive-url=https://web.archive.org/web/20171201032201/http://exoplanet.eu/catalog/gj_667_c_d/|archive-date=2017-12-01}}</ref><ref>{{cite web |url=http://exoplanet.eu/catalog/gj_667_c_h/ |title=GJ 667 C h |website=The Extrasolar Planet Encyclopaedia |publisher=Exoplanet.eu |date=2016-02-23 |access-date=2018-03-22 |url-status=live |archive-url=https://web.archive.org/web/20171201041119/http://exoplanet.eu/catalog/gj_667_c_h/ |archive-date=2017-12-01 }}</ref><ref name="Barnes2019"/> | rowspan = "2"|5 dubious candidates<br><ref>{{cite web|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=GJ+667+C |title=GJ 667 C |website=NASA Exoplanet Science Institute|publisher=California Institute of Technology|access-date=2018-03-22}}</ref><ref name=PHL/><ref>{{cite encyclopedia|url=https://exoplanet.eu/catalog/gj_667_c_d--1090/|title=GJ 667 C d|access-date=2018-03-22|url-status=live|archive-url=https://web.archive.org/web/20171201032201/http://exoplanet.eu/catalog/gj_667_c_d/|encyclopedia=]|archive-date=2017-12-01}}</ref><ref>{{cite encyclopedia |url=https://exoplanet.eu/catalog/gj_667_c_h--1296/ |title=GJ 667 C h |date=2016-02-23 |access-date=2018-03-22 |url-status=live |archive-url=https://web.archive.org/web/20171201041119/http://exoplanet.eu/catalog/gj_667_c_h/ |encyclopedia=] |archive-date=2017-12-01 }}</ref><ref name="Barnes2019"/>
|- style="background:#BCD4E6;" |- style="background:#BCD4E6;"
| {{sort|c3|]}}<sup>↑</sup> || {{sort|0003.9000|≥3.9}} || — || 0.1251 || {{sort|0028|28.2}} || 0.03 || ''~52?'' || ] || 2011 | {{sort|c3|]}}<sup>↑</sup> || {{sort|0003.9000|≥3.9}} || — || 0.1251 || {{sort|0028|28.2}} || 0.03 || ''~52?'' || ] || 2011
Line 371: Line 400:
| ] || {{sort|0005.2000|≥5.2}} || — || 0.421 || 140 || 0.45 || — || ] || 2022 | ] || {{sort|0005.2000|≥5.2}} || — || 0.421 || 140 || 0.45 || — || ] || 2022
| <ref>{{cite journal |last1=Damasso |first1=M. |last2=Perger |first2=M. |last3=Almenara |first3=J. M. |last4=Nardiello |first4=D. |last5=Pérez-Torres |first5=M. |last6=Sozzetti |first6=A. |last7=Hara |first7=N. C. |last8=Quirrenbach |first8=A. |last9=Bonfils |first9=X. |last10=Osorio |first10=M. R. Zapatero |last11=Astudillo-Defru |first11=N. |last12=Hernández |first12=J. I. González |last13=Mascareño |first13=A. Suárez |last14=Amado |first14=P. J. |last15=Forveille |first15=T. |last16=Lillo-Box |first16=J. |last17=Alibert |first17=Y. |last18=Caballero |first18=J. A. |last19=Cifuentes |first19=C. |last20=Delfosse |first20=X. |last21=Figueira |first21=P. |last22=Galadí-Enríquez |first22=D. |last23=Hatzes |first23=A. P. |last24=Henning |first24=Th |last25=Kaminski |first25=A. |last26=Mayor |first26=M. |last27=Murgas |first27=F. |last28=Montes |first28=D. |last29=Pinamonti |first29=M. |last30=Reiners |first30=A. |last31=Ribas |first31=I. |last32=Béjar |first32=V. J. S. |last33=Schweitzer |first33=A. |last34=Zechmeister |first34=M. |title=A quarter century of spectroscopic monitoring of the nearby M dwarf Gl 514 |journal=Astronomy & Astrophysics |date=13 April 2022 |volume=666 |pages=A187 |doi=10.1051/0004-6361/202243522 |arxiv=2204.06376 |s2cid=248157318 }}</ref> | <ref>{{cite journal |last1=Damasso |first1=M. |last2=Perger |first2=M. |last3=Almenara |first3=J. M. |last4=Nardiello |first4=D. |last5=Pérez-Torres |first5=M. |last6=Sozzetti |first6=A. |last7=Hara |first7=N. C. |last8=Quirrenbach |first8=A. |last9=Bonfils |first9=X. |last10=Osorio |first10=M. R. Zapatero |last11=Astudillo-Defru |first11=N. |last12=Hernández |first12=J. I. González |last13=Mascareño |first13=A. Suárez |last14=Amado |first14=P. J. |last15=Forveille |first15=T. |last16=Lillo-Box |first16=J. |last17=Alibert |first17=Y. |last18=Caballero |first18=J. A. |last19=Cifuentes |first19=C. |last20=Delfosse |first20=X. |last21=Figueira |first21=P. |last22=Galadí-Enríquez |first22=D. |last23=Hatzes |first23=A. P. |last24=Henning |first24=Th |last25=Kaminski |first25=A. |last26=Mayor |first26=M. |last27=Murgas |first27=F. |last28=Montes |first28=D. |last29=Pinamonti |first29=M. |last30=Reiners |first30=A. |last31=Ribas |first31=I. |last32=Béjar |first32=V. J. S. |last33=Schweitzer |first33=A. |last34=Zechmeister |first34=M. |title=A quarter century of spectroscopic monitoring of the nearby M dwarf Gl 514 |journal=Astronomy & Astrophysics |date=13 April 2022 |volume=666 |pages=A187 |doi=10.1051/0004-6361/202243522 |arxiv=2204.06376 |s2cid=248157318 }}</ref>

|-
! scope="row" style="background:#F8F9FA; font-weight:normal; padding-right:0.4em;" | ]
| 26.231 || {{sort|1401|14.01}} || 0.164
| ] || {{sort|0010.6200|≥10.6}} || — || 0.571 || 390 || — || — || ] || 2023
| 1 refuted candidate<ref>{{cite journal |last1=Vedantham |first1=H. K. |last2=Callingham |first2=J. R. |last3=Shimwell |first3=T. W. |last4=Tasse |first4=C. |last5=Pope |first5=B. J. S. |last6=Bedell |first6=M. |last7=Snellen |first7=I. |last8=Best |first8=P. |last9=Hardcastle |first9=M. J. |last10=Haverkorn |first10=M. |last11=Mechev |first11=A. |last12=O’Sullivan |first12=S. P. |last13=Röttgering |first13=H. J. A. |last14=White |first14=G. J. |title=Coherent radio emission from a quiescent red dwarf indicative of star–planet interaction |journal=Nature Astronomy |date=June 2020 |volume=4 |issue=6 |pages=577–583 |doi=10.1038/s41550-020-1011-9 |arxiv=2002.08727 |bibcode=2020NatAs...4..577V |s2cid=211204712 }}</ref><ref>{{cite journal |author1-link=Suvrath Mahadevan |last1=Mahadevan |first1=Suvrath |last2=Stefánsson |first2=Guðmundur |last3=Robertson |first3=Paul |last4=Terrien |first4=Ryan C. |last5=Ninan |first5=Joe P. |last6=Holcomb |first6=Rae J. |last7=Halverson |first7=Samuel |last8=Cochran |first8=William D. |last9=Kanodia |first9=Shubham |last10=Ramsey |first10=Lawrence W. |last11=Wolszczan |first11=Alexander |last12=Endl |first12=Michael |last13=Bender |first13=Chad F. |last14=Diddams |first14=Scott A. |last15=Fredrick |first15=Connor |last16=Hearty |first16=Fred |last17=Monson |first17=Andrew |last18=Metcalf |first18=Andrew J. |last19=Roy |first19=Arpita |last20=Schwab |first20=Christian |title=The Habitable-zone Planet Finder Detects a Terrestrial-mass Planet Candidate Closely Orbiting Gliese 1151: The Likely Source of Coherent Low-frequency Radio Emission from an Inactive Star |journal=The Astrophysical Journal Letters |date=3 February 2021 |volume=919 |issue=1 |pages=L9 |doi=10.3847/2041-8213/abe2b2 |arxiv=2102.02233 |bibcode=2021ApJ...919L...9M |s2cid=231802021 |doi-access=free }}</ref><ref name=Perger2021/><ref name="Blanco-Pozo2023"/>


|- |-
! scope="row" style="background:#F8F9FA; font-weight:normal; padding-right:0.4em;" | ] ! scope="row" style="background:#F8F9FA; font-weight:normal; padding-right:0.4em;" | ]
| 26.351 || {{sort|1139.5|11.395}} || 0.32 | 26.351 || {{sort|1139.5|11.395}} || 0.32
| ] || {{sort|0002.8200|2.8}} || 1.31 || 0.0173 || {{sort|0001.47|1.47}} || {{sort|0|<0.05}} || 88.4 || ] || 2021 | <small>{{sort|b0|]}}</small> || {{sort|0002.8200|2.8}} || 1.31 || 0.0173 || {{sort|0001.47|1.47}} || {{sort|0|<0.05}} || 88.4 || ] || 2021
| <ref>{{cite journal |last1=Trifonov |first1=T. |last2=Caballero |first2=J. A. |last3=Morales |first3=J. C. |last4=Seifahrt |first4=A. |last5=Ribas |first5=I. |last6=Reiners |first6=Ansgar |last7=Bean |first7=J. L. |last8=Luque |first8=R. |last9=Parviainen |first9=H. |last10=Pallé |first10=E. |last11=Stock |first11=S. |last12=Zechmeister |first12=M. |last13=Amado |first13=P. J. |last14=Anglada-Escudé |first14=G. |last15=Azzaro |first15=M. |last16=Barclay |first16=T. |last17=Béjar |first17=V. J. S. |last18=Bluhm |first18=P. |last19=Casasayas-Barris |first19=N. |last20=Cifuentes |first20=C. |last21=Collins |first21=K. A. |last22=Collins |first22=K. I. |last23=Cortés-Contreras |first23=M. |last24=de Leon |first24=J. |last25=Dreizler |first25=S. |last26=Dressing |first26=C. D. |last27=Esparza-Borges |first27=E. |last28=Espinoza |first28=N. |last29=Fausnaugh |first29=M. |last30=Fukui |first30=A. |last31=Hatzes |first31=A. P. |last32=Hellier |first32=C. |last33=Henning |first33=Th. |last34=Henze |first34=C. E. |last35=Herrero |first35=E. |last36=Jeffers |first36=S. V. |last37=Jenkins |first37=J. M. |last38=Jensen |first38=E. L. N. |last39=Kaminski |first39=A. |last40=Kasper |first40=D. |last41=Kossakowski |first41=D. |last42=Kürster |first42=M. |last43=Lafarga |first43=M. |last44=Latham |first44=D. W. |last45=Mann |first45=A. W. |last46=Molaverdikhani |first46=K. |last47=Montes |first47=D. |last48=Montet |first48=B. T. |last49=Murgas |first49=F. |last50=Narita |first50=N. |last51=Oshagh |first51=M. |last52=Passegger |first52=V. M. |last53=Pollacco |first53=D. |last54=Quinn |first54=S. N. |last55=Quirrenbach |first55=A. |last56=Ricker |first56=G. R. |last57=Rodríguez López |first57=C. |last58=Sanz-Forcada |first58=J. |last59=Schwarz |first59=R. P. |last60=Schweitzer |first60=A. |last61=Seager |first61=S. |last62=Shporer |first62=A. |last63=Stangret |first63=M. |last64=Stürmer |first64=J. |last65=Tan |first65=T. G. |last66=Tenenbaum |first66=P. |last67=Twicken |first67=J. D. |last68=Vanderspek |first68=R. |last69=Winn |first69=J. N. |title=A nearby transiting rocky exoplanet that is suitable for atmospheric investigation |journal=Science |date=5 March 2021 |volume=371 |issue=6533 |pages=1038–1041 |doi=10.1126/science.abd7645 |pmid=33674491 |arxiv=2103.04950 |bibcode=2021Sci...371.1038T |s2cid=232124642 }}</ref> | <ref>{{cite journal |last1=Trifonov |first1=T. |last2=Caballero |first2=J. A. |last3=Morales |first3=J. C. |last4=Seifahrt |first4=A. |last5=Ribas |first5=I. |last6=Reiners |first6=Ansgar |last7=Bean |first7=J. L. |last8=Luque |first8=R. |last9=Parviainen |first9=H. |last10=Pallé |first10=E. |last11=Stock |first11=S. |last12=Zechmeister |first12=M. |last13=Amado |first13=P. J. |last14=Anglada-Escudé |first14=G. |last15=Azzaro |first15=M. |last16=Barclay |first16=T. |last17=Béjar |first17=V. J. S. |last18=Bluhm |first18=P. |last19=Casasayas-Barris |first19=N. |last20=Cifuentes |first20=C. |last21=Collins |first21=K. A. |last22=Collins |first22=K. I. |last23=Cortés-Contreras |first23=M. |last24=de Leon |first24=J. |last25=Dreizler |first25=S. |last26=Dressing |first26=C. D. |last27=Esparza-Borges |first27=E. |last28=Espinoza |first28=N. |last29=Fausnaugh |first29=M. |last30=Fukui |first30=A. |last31=Hatzes |first31=A. P. |last32=Hellier |first32=C. |last33=Henning |first33=Th. |last34=Henze |first34=C. E. |last35=Herrero |first35=E. |last36=Jeffers |first36=S. V. |last37=Jenkins |first37=J. M. |last38=Jensen |first38=E. L. N. |last39=Kaminski |first39=A. |last40=Kasper |first40=D. |last41=Kossakowski |first41=D. |last42=Kürster |first42=M. |last43=Lafarga |first43=M. |last44=Latham |first44=D. W. |last45=Mann |first45=A. W. |last46=Molaverdikhani |first46=K. |last47=Montes |first47=D. |last48=Montet |first48=B. T. |last49=Murgas |first49=F. |last50=Narita |first50=N. |last51=Oshagh |first51=M. |last52=Passegger |first52=V. M. |last53=Pollacco |first53=D. |last54=Quinn |first54=S. N. |last55=Quirrenbach |first55=A. |last56=Ricker |first56=G. R. |last57=Rodríguez López |first57=C. |last58=Sanz-Forcada |first58=J. |last59=Schwarz |first59=R. P. |last60=Schweitzer |first60=A. |last61=Seager |first61=S. |last62=Shporer |first62=A. |last63=Stangret |first63=M. |last64=Stürmer |first64=J. |last65=Tan |first65=T. G. |last66=Tenenbaum |first66=P. |last67=Twicken |first67=J. D. |last68=Vanderspek |first68=R. |last69=Winn |first69=J. N. |title=A nearby transiting rocky exoplanet that is suitable for atmospheric investigation |journal=Science |date=5 March 2021 |volume=371 |issue=6533 |pages=1038–1041 |doi=10.1126/science.abd7645 |pmid=33674491 |arxiv=2103.04950 |bibcode=2021Sci...371.1038T |s2cid=232124642 }}</ref>
<!-- <!--
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| ] || {{sort|0007.1000|≥7.1}} || — || 0.097 || {{sort|0015.5|15.5}} || 0.04 || — || ] || 2019 | ] || {{sort|0007.1000|≥7.1}} || — || 0.097 || {{sort|0015.5|15.5}} || 0.04 || — || ] || 2019
| <ref name="GJ686b"/><ref name="Barnes2019"/> | <ref name="GJ686b"/><ref name="Barnes2019"/>

|-
! scope="row" style="background:#F8F9FA; font-weight:normal; padding-right:0.4em;" | ]
| 27.275 || 12.67<ref>{{Cite simbad|title=GJ 1289}}</ref> || 0.21
| ] || {{sort|0006.27|≥6.3}} || — || 0.27 || 112 || 0 || — || ] || 2024
| <ref name="Moutou2024"/>


|- style="background:#ffffb0;" |- style="background:#ffffb0;"
! scope="row" rowspan="2" style="background:#FFFFB0; font-weight:normal; padding-right:0.4em;" |]<sup>#</sup> ! scope="row" rowspan="3" style="background:#FFFFB0; font-weight:normal; padding-right:0.4em;" |]<sup>#</sup>
| rowspan = "2"|27.836 ||rowspan = "2"|{{sort|0474|4.74}} ||rowspan = "2"|0.95 | rowspan = "3"|27.836 ||rowspan = "3"|{{sort|0474|4.74}} ||rowspan = "3"|0.95
| ] || {{sort|0005.1000|≥5.1}} || — || 0.0502 || {{sort|00042|4.22}} || {{sort|0.12|~0.1}} || ''~77?'' || ] || 2009 | ] || {{sort|0006.1000|≥6.1}} || — || 0.05 || {{sort|0004.215|4.22}} || 0.05 || ''~77?'' || ] || 2009
|rowspan = "3"|a debris ]<ref name="Cretignier2023"/>
|rowspan = "2"|a debris ],<ref>{{cite web|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=61+Vir |title=61 Vir |website=NASA Exoplanet Science Institute|publisher=California Institute of Technology|access-date=2018-03-22}}</ref> 1 disputed candidate<ref name=Rosenthal2021/>
|- style="background:#ffffb0;" |- style="background:#ffffb0;"
| ] || {{sort|0018.2000|≥18}} || — || 0.218 || {{sort|0038|38.0}} || 0.14 || ''~77?'' || ] || 2009 | ] || {{sort|0017.9000|≥17.9}} || — || 0.22 || {{sort|0038.09|38.1}} || 0.06 || ''~77?'' || ] || 2009
|- style="background:#ffffb0;"
| ] || {{sort|0010.5000|≥10.5}} || — || 0.47 || {{sort|0123.2|123}} || 0.12 || ''~77?'' || ] || 2009


|- |-
Line 443: Line 486:
|<ref>{{cite web|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=HD+102365 |title=HD 102365 |website=NASA Exoplanet Science Institute|publisher=California Institute of Technology|access-date=2018-03-22}}</ref> |<ref>{{cite web|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=HD+102365 |title=HD 102365 |website=NASA Exoplanet Science Institute|publisher=California Institute of Technology|access-date=2018-03-22}}</ref>


|- style="background:#ffffb0;"
|-
! scope="row" style="background:#F8F9FA; font-weight:normal; padding-right:0.4em;" | ] ! scope="row" rowspan="3" style="background:#FFFFB0; font-weight:normal; padding-right:0.4em;" | ]<sup>#</sup>
| 30.719 ||{{sort|0998|9.98}} ||0.45 | rowspan="3"|30.719 || rowspan="3"|{{sort|0998|9.98}} || rowspan="3"|0.45
| ] || {{sort|0000.5460|0.55}} || 0.72 || 0.0071 || {{sort|0000.321962|0.32}} || 0 || 80.75 || ] || 2021 | <small>{{sort|b0|]}}</small> || {{sort|0000.6330|0.63}} || 0.70 || 0.0071 || {{sort|0000.3219225|0.322}} || 0.06 || 79.89 || ] || 2021
|<ref>{{cite journal |last1=Lam |first1=Kristine W. F. |last2=Csizmadia |first2=Szilárd |last3=Astudillo-Defru |first3=Nicola |last4=Bonfils |first4=Xavier |last5=Gandolfi |first5=Davide |last6=Padovan |first6=Sebastiano |last7=Esposito |first7=Massimiliano |last8=Hellier |first8=Coel |last9=Hirano |first9=Teruyuki |last10=Livingston |first10=John |last11=Murgas |first11=Felipe |last12=Smith |first12=Alexis M. S. |last13=Collins |first13=Karen A. |last14=Mathur |first14=Savita |last15=Garcia |first15=Rafael A. |last16=Howell |first16=Steve B. |last17=Santos |first17=Nuno C. |last18=Dai |first18=Fei |last19=Ricker |first19=George R. |last20=Vanderspek |first20=Roland |last21=Latham |first21=David W. |last22=Seager |first22=Sara |last23=Winn |first23=Joshua N. |last24=Jenkins |first24=Jon M. |last25=Albrecht |first25=Simon |last26=Almenara |first26=Jose M. |last27=Artigau |first27=Etienne |last28=Barragán |first28=Oscar |last29=Bouchy |first29=François |last30=Cabrera |first30=Juan |last31=Charbonneau |first31=David |last32=Chaturvedi |first32=Priyanka |last33=Chaushev |first33=Alexander |last34=Christiansen |first34=Jessie L. |last35=Cochran |first35=William D. |last36=De Meideiros |first36=José R. |last37=Delfosse |first37=Xavier |last38=Díaz |first38=Rodrigo F. |last39=Doyon |first39=René |last40=Eigmüller |first40=Philipp |last41=Figueira |first41=Pedro |last42=Forveille |first42=Thierry |last43=Fridlund |first43=Malcolm |last44=Gaisné |first44=Guillaume |last45=Goffo |first45=Elisa |last46=Georgieva |first46=Iskra |last47=Grziwa |first47=Sascha |last48=Guenther |first48=Eike |last49=Hatzes |first49=Artie P. |last50=Johnson |first50=Marshall C. |last51=Kabáth |first51=Petr |last52=Knudstrup |first52=Emil |last53=Korth |first53=Judith |last54=Lewin |first54=Pablo |last55=Lissauer |first55=Jack J. |last56=Lovis |first56=Christophe |last57=Luque |first57=Rafael |last58=Melo |first58=Claudio |last59=Morgan |first59=Edward H. |last60=Morris |first60=Robert |last61=Mayor |first61=Michel |last62=Narita |first62=Norio |last63=Osborne |first63=Hannah L. M. |last64=Palle |first64=Enric |last65=Pepe |first65=Francesco |last66=Persson |first66=Carina M. |last67=Quinn |first67=Samuel N. |last68=Rauer |first68=Heike |last69=Redfield |first69=Seth |last70=Schlieder |first70=Joshua E. |last71=Ségransan |first71=Damien |last72=Serrano |first72=Luisa M. |last73=Smith |first73=Jeffrey C. |last74=Šubjak |first74=Ján |last75=Twicken |first75=Joseph D. |last76=Udry |first76=Stéphane |last77=Van Eylen |first77=Vincent |last78=Vezie |first78=Michael |title=GJ 367b: A dense, ultrashort-period sub-Earth planet transiting a nearby red dwarf star |journal=Science |date=3 December 2021 |volume=374 |issue=6572 |pages=1271–1275 |doi=10.1126/science.aay3253|pmid=34855492 |arxiv=2112.01309 |bibcode=2021Sci...374.1271L |s2cid=244799656 |url=https://eprints.keele.ac.uk/10383/1/2112.01309.pdf }}</ref> | rowspan="3"|<ref>{{cite journal |last1=Lam |first1=Kristine W. F. |last2=Csizmadia |first2=Szilárd |last3=Astudillo-Defru |first3=Nicola |last4=Bonfils |first4=Xavier |last5=Gandolfi |first5=Davide |last6=Padovan |first6=Sebastiano |last7=Esposito |first7=Massimiliano |last8=Hellier |first8=Coel |last9=Hirano |first9=Teruyuki |last10=Livingston |first10=John |last11=Murgas |first11=Felipe |last12=Smith |first12=Alexis M. S. |last13=Collins |first13=Karen A. |last14=Mathur |first14=Savita |last15=Garcia |first15=Rafael A. |last16=Howell |first16=Steve B. |last17=Santos |first17=Nuno C. |last18=Dai |first18=Fei |last19=Ricker |first19=George R. |last20=Vanderspek |first20=Roland |last21=Latham |first21=David W. |last22=Seager |first22=Sara |last23=Winn |first23=Joshua N. |last24=Jenkins |first24=Jon M. |last25=Albrecht |first25=Simon |last26=Almenara |first26=Jose M. |last27=Artigau |first27=Etienne |last28=Barragán |first28=Oscar |last29=Bouchy |first29=François |last30=Cabrera |first30=Juan |last31=Charbonneau |first31=David |last32=Chaturvedi |first32=Priyanka |last33=Chaushev |first33=Alexander |last34=Christiansen |first34=Jessie L. |last35=Cochran |first35=William D. |last36=De Meideiros |first36=José R. |last37=Delfosse |first37=Xavier |last38=Díaz |first38=Rodrigo F. |last39=Doyon |first39=René |last40=Eigmüller |first40=Philipp |last41=Figueira |first41=Pedro |last42=Forveille |first42=Thierry |last43=Fridlund |first43=Malcolm |last44=Gaisné |first44=Guillaume |last45=Goffo |first45=Elisa |last46=Georgieva |first46=Iskra |last47=Grziwa |first47=Sascha |last48=Guenther |first48=Eike |last49=Hatzes |first49=Artie P. |last50=Johnson |first50=Marshall C. |last51=Kabáth |first51=Petr |last52=Knudstrup |first52=Emil |last53=Korth |first53=Judith |last54=Lewin |first54=Pablo |last55=Lissauer |first55=Jack J. |last56=Lovis |first56=Christophe |last57=Luque |first57=Rafael |last58=Melo |first58=Claudio |last59=Morgan |first59=Edward H. |last60=Morris |first60=Robert |last61=Mayor |first61=Michel |last62=Narita |first62=Norio |last63=Osborne |first63=Hannah L. M. |last64=Palle |first64=Enric |last65=Pepe |first65=Francesco |last66=Persson |first66=Carina M. |last67=Quinn |first67=Samuel N. |last68=Rauer |first68=Heike |last69=Redfield |first69=Seth |last70=Schlieder |first70=Joshua E. |last71=Ségransan |first71=Damien |last72=Serrano |first72=Luisa M. |last73=Smith |first73=Jeffrey C. |last74=Šubjak |first74=Ján |last75=Twicken |first75=Joseph D. |last76=Udry |first76=Stéphane |last77=Van Eylen |first77=Vincent |last78=Vezie |first78=Michael |title=GJ 367b: A dense, ultrashort-period sub-Earth planet transiting a nearby red dwarf star |journal=Science |date=3 December 2021 |volume=374 |issue=6572 |pages=1271–1275 |doi=10.1126/science.aay3253|pmid=34855492 |arxiv=2112.01309 |bibcode=2021Sci...374.1271L |s2cid=244799656 |url=https://eprints.keele.ac.uk/10383/1/2112.01309.pdf }}</ref><ref name="Goffo2023"/>
|- style="background:#ffffb0;"
| ] || {{sort|0004.1300|≥4.1}} || — || 0.077 || 11.5 || 0.09 || ''~80?'' || ] || 2023
|- style="background:#ffffb0;"
| ] || {{sort|0006.0300|≥6.0}} || — || 0.159 || 34.4 || 0.14 || ''~80?'' || ] || 2023


|- style="background:#ffffb0;" |- style="background:#ffffb0;"
Line 455: Line 502:
|rowspan="3"|<ref name="GL357system"/><ref name="Barnes2019"/> |rowspan="3"|<ref name="GL357system"/><ref name="Barnes2019"/>
|- style="background:#ffffb0;" |- style="background:#ffffb0;"
| ] || {{sort|0003.6000|≥3.6}} || — || 0.061 || 9.13 || 0.04 || ~89? || ] || 2019 | ] || {{sort|0003.6000|≥3.6}} || — || 0.061 || 9.13 || 0.04 || ''~89?'' || ] || 2019
|- style="background:#BCD4E6;" |- style="background:#BCD4E6;"
| ]<sup>↑</sup> || {{sort|0007.7000|≥7.7}} || — || 0.204 || 55.7 || 0.03 || ~89? || ] || 2019 | ]<sup>↑</sup> || {{sort|0007.7000|≥7.7}} || — || 0.204 || 55.7 || 0.03 || ''~89?'' || ] || 2019


|- <!-- HD 285968 --> |- <!-- HD 285968 -->
Line 463: Line 510:
| 30.937 || {{sort|1010|10.1}} || 0.45 | 30.937 || {{sort|1010|10.1}} || 0.45
| ] || {{sort|0008.0000|≥8.0}} || — || 0.066 || {{sort|0008.77|8.77}} || 0.08 || — || ] || 2007 | ] || {{sort|0008.0000|≥8.0}} || — || 0.066 || {{sort|0008.77|8.77}} || 0.08 || — || ] || 2007
| 1 disputed candidate<ref>{{cite web|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=HD+285968 |title=HD 285968 |website=NASA Exoplanet Science Institute|publisher=California Institute of Technology |access-date=2018-03-22}}</ref><ref>{{cite web |url=http://exoplanet.eu/catalog/gj_176_c/ |website=The Extrasolar Planet Encyclopaedia |title=GJ 176 c |publisher=Exoplanet.eu |date=2010-12-17 |access-date=2014-05-20 |url-status=live |archive-url=https://web.archive.org/web/20140223071946/http://exoplanet.eu/catalog/gj_176_c/ |archive-date=2014-02-23 }}</ref><ref name="Barnes2019"/> | 1 disputed candidate<ref>{{cite web|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=HD+285968 |title=HD 285968 |website=NASA Exoplanet Science Institute|publisher=California Institute of Technology |access-date=2018-03-22}}</ref><ref>{{cite encyclopedia |url=https://exoplanet.eu/catalog/gj_176_c--786/ |title=GJ 176 c |date=2010-12-17 |access-date=2014-05-20 |url-status=live |archive-url=https://web.archive.org/web/20140223071946/http://exoplanet.eu/catalog/gj_176_c/ |encyclopedia=] |archive-date=2014-02-23 }}</ref><ref name="Barnes2019"/>
<!-- <!--
|- |-
Line 489: Line 536:
| rowspan="2"| 31.683 || rowspan="2"| {{sort|0863|8.63}} || rowspan="2"| 0.50 | rowspan="2"| 31.683 || rowspan="2"| {{sort|0863|8.63}} || rowspan="2"| 0.50
| ] || {{sort|0017.0000|17}} || 4.38 || 0.0645 || {{sort|0008.4629991|8.463}} || 0.10 || 89.03 || ] || 2020 | ] || {{sort|0017.0000|17}} || 4.38 || 0.0645 || {{sort|0008.4629991|8.463}} || 0.10 || 89.03 || ] || 2020
| rowspan="2"| <ref>{{cite journal |first1=Peter |last1=Plavchan |first2=Thomas |last2=Barclay |first3=Jonathan |last3=Gagné |display-authors=etal |title=A planet within the debris disk around the pre-main-sequence star AU Microscopii |journal=Nature |year=2020 |volume=582 |issue=7813 |pages=497–500 |doi=10.1038/s41586-020-2400-z |pmid=32581383 |pmc=7323865 |arxiv=2006.13248|bibcode=2020Natur.582..497P |s2cid=220042005 }}</ref><ref>{{cite journal |last=Martioli |first=E. |display-authors=etal |arxiv=2012.13238 |title=New constraints on the planetary system around the young active star AU Mic. Two transiting warm Neptunes near mean-motion resonance |journal=Astronomy & Astrophysics |year=2021 |volume=A177 |page=649 |doi=10.1051/0004-6361/202040235 |bibcode=2021A&A...649A.177M |s2cid=229371309 }}</ref> | rowspan="2"| 2 candidates<ref>{{cite journal |first1=Peter |last1=Plavchan |first2=Thomas |last2=Barclay |first3=Jonathan |last3=Gagné |display-authors=etal |title=A planet within the debris disk around the pre-main-sequence star AU Microscopii |journal=Nature |year=2020 |volume=582 |issue=7813 |pages=497–500 |doi=10.1038/s41586-020-2400-z |pmid=32581383 |pmc=7323865 |arxiv=2006.13248|bibcode=2020Natur.582..497P |s2cid=220042005 }}</ref><ref>{{cite journal |last=Martioli |first=E. |display-authors=etal |arxiv=2012.13238 |title=New constraints on the planetary system around the young active star AU Mic. Two transiting warm Neptunes near mean-motion resonance |journal=Astronomy & Astrophysics |year=2021 |volume=A177 |page=649 |doi=10.1051/0004-6361/202040235 |bibcode=2021A&A...649A.177M |s2cid=229371309 }}</ref><ref name="Wittrock2023"/><ref name="Donati2023"/>
|- style="background:#ffffb0;" |- style="background:#ffffb0;"
| ] || {{sort|0028.0000|<28}} || 3.51 || 0.1101 || {{sort|18.858991|18.86}} || 0 || 88.62 || ] || 2020 | ] || {{sort|0028.0000|<28}} || 3.51 || 0.1101 || {{sort|18.858991|18.86}} || 0 || 88.62 || ] || 2020
Line 496: Line 543:
! scope="row" style="background:#F8F9FA; font-weight:normal; padding-right:0.4em;" | ] ! scope="row" style="background:#F8F9FA; font-weight:normal; padding-right:0.4em;" | ]
| 31.882 || {{sort|1067|10.67}} || 0.41 | 31.882 || {{sort|1067|10.67}} || 0.41
| ] || {{sort|0021.3600|21.4}} || 4.33 || 0.0280 || 2.64 || 0.15 || 85.8 || ] || 2004 | <small>{{sort|b0|]}}</small> || {{sort|0021.3600|21.4}} || 4.33 || 0.0280 || 2.64 || 0.15 || 85.8 || ] || 2004
| <ref>{{cite journal | bibcode = 2007A&A...472L..13G | author = Gillon, M. | display-authors = etal | title = Detection of transits of the nearby hot Neptune GJ 436 b | journal = Astronomy and Astrophysics | volume = 472 | issue = 2 | pages = L13–L16 | date = 2007 | doi = 10.1051/0004-6361:20077799|arxiv = 0705.2219 | s2cid = 13552824 }}</ref><ref name="Lanotte2014"/> | <ref>{{cite journal | bibcode = 2007A&A...472L..13G | author = Gillon, M. | display-authors = etal | title = Detection of transits of the nearby hot Neptune GJ 436 b | journal = Astronomy and Astrophysics | volume = 472 | issue = 2 | pages = L13–L16 | date = 2007 | doi = 10.1051/0004-6361:20077799|arxiv = 0705.2219 | s2cid = 13552824 }}</ref><ref name="Lanotte2014"/>


Line 504: Line 551:
| ] || {{sort|0016.4000|≥16.4}} || — || 0.106 || 17.3 || 0.03 || — || ] || 2019 | ] || {{sort|0016.4000|≥16.4}} || — || 0.106 || 17.3 || 0.03 || — || ] || 2019
| <ref name="Perger2019"/> | <ref name="Perger2019"/>

|-
! scope="row" style="background:#F8F9FA; font-weight:normal; padding-right:0.4em;" | ]
| 32.316 || {{Sort|1363|13.6}} || 0.184
| ] || {{sort|0003.6900|≥3.7}} || — || 0.0405 || 6.944 || 0 || — || ] || 2023
| <ref name="Gorrini2023"/>


|- style="background:#ffffb0;" |- style="background:#ffffb0;"
Line 516: Line 569:
|} |}


===Excluded objects=== ==Excluded objects==
Unlike for bodies within the ], there is no clearly established method for officially recognizing an exoplanet. According to the ], an exoplanet should be considered confirmed if it has not been disputed for five years after its discovery.<ref>{{cite web |url=http://www.techtimes.com/articles/77119/20150818/want-to-name-an-exoplanet-heres-your-chance.htm |first=Rhodi |last=Lee |title=Want To Name An Exoplanet? Here's Your Chance |publisher=Tech Times |date=2015-09-18 |access-date=2015-09-17 |url-status=live |archive-url=https://web.archive.org/web/20150907115335/http://www.techtimes.com/articles/77119/20150818/want-to-name-an-exoplanet-heres-your-chance.htm |archive-date=2015-09-07 }}</ref> There have been examples where the existence of exoplanets has been proposed, but even after follow-up studies their existence is still considered doubtful by some astronomers. Such cases include ] (7.9 ly, in 2019),<ref name="Barnes2019"/> ] (15.8 ly, in 2007),<ref>{{cite journal| doi=10.1086/599044| title=A Search for Astrometric Companions to Stars in the Southern Hemisphere| journal=Publications of the Astronomical Society of the Pacific| volume=121| issue=878| page=365| year=2009| last1=Bartlett| first1=Jennifer L|author1-link=Jennifer Bartlett (astronomer)| last2=Ianna| first2=Philip A| last3=Begam| first3=Michael C| bibcode=2009PASP..121..365B| s2cid=122529477| doi-access=}}</ref> Unlike for bodies within the ], there is no clearly established method for officially recognizing an exoplanet. According to the ], an exoplanet should be considered confirmed if it has not been disputed for five years after its discovery.<ref>{{cite web |url=http://www.techtimes.com/articles/77119/20150818/want-to-name-an-exoplanet-heres-your-chance.htm |first=Rhodi |last=Lee |title=Want To Name An Exoplanet? Here's Your Chance |publisher=Tech Times |date=2015-09-18 |access-date=2015-09-17 |url-status=live |archive-url=https://web.archive.org/web/20150907115335/http://www.techtimes.com/articles/77119/20150818/want-to-name-an-exoplanet-heres-your-chance.htm |archive-date=2015-09-07 }}</ref> There have been examples where the existence of exoplanets has been proposed, but even after follow-up studies their existence is still considered doubtful by some astronomers. Such cases include ] (7.9 ly, in 2019),<ref name="Barnes2019"/> ] (15.8 ly, in 2007),<ref>{{cite journal| doi=10.1086/599044| title=A Search for Astrometric Companions to Stars in the Southern Hemisphere| journal=Publications of the Astronomical Society of the Pacific| volume=121| issue=878| page=365| year=2009| last1=Bartlett| first1=Jennifer L|author1-link=Jennifer Bartlett (astronomer)| last2=Ianna| first2=Philip A| last3=Begam| first3=Michael C| bibcode=2009PASP..121..365B| s2cid=122529477| doi-access=}}</ref>
and ] (16.3 ly, in 2014).<ref name="Feng2020" />
] (16.3 ly, in 2014),<!--<ref name=PHL/><ref>{{cite web |url=http://exoplanet.eu/catalog/gj_682_b/ |website=The Extrasolar Planet Encyclopaedia |title=GJ 682 b |publisher=Exoplanet.eu |access-date=2015-03-30 |url-status=live |archive-url=https://web.archive.org/web/20150402132202/http://exoplanet.eu/catalog/gj_682_b/ |archive-date=2015-04-02 }}</ref><ref>{{cite web |url=http://exoplanet.eu/catalog/gj_682_c/ |website=The Extrasolar Planet Encyclopaedia |title=GJ 682 c |publisher=Exoplanet.eu |access-date=2015-03-30 |url-status=live |archive-url=https://web.archive.org/web/20150402093100/http://exoplanet.eu/catalog/gj_682_c/ |archive-date=2015-04-02 }}</ref>--><ref name="Feng2020" />
There are also several instances where proposed exoplanets were later disproved by subsequent studies, including candidates around ] B (4.36 ly),<!--<ref>{{cite web |url=https://exoplanet.eu/catalog/alf_cen_b_b--1215/ |title=alf Cen B b |date=2011-05-27 |access-date=2014-05-17 |url-status=live |archive-url=https://web.archive.org/web/20140625075606/http://exoplanet.eu/catalog/alf_cen_b_b/ |work=] |archive-date=2014-06-25 }}</ref><ref>{{cite web |url=http://www.drewexmachina.com/2015/03/28/has-another-planet-been-found-orbiting-alpha-centauri-b/ |title=Has Another Planet Been Found Orbiting Alpha Centauri B? |first=Andrew |last=LePage |publisher=Drew Ex Machina |date=2015-03-28 |access-date=2015-09-17 |url-status=live |archive-url=https://web.archive.org/web/20150929103322/http://www.drewexmachina.com/2015/03/28/has-another-planet-been-found-orbiting-alpha-centauri-b/ |archive-date=2015-09-29 }}</ref>--><ref name="Rajpaul"/>
] A (16.3 ly, in 2018),<ref>{{cite journal |last1=Ma |first1=Bo |last2=Ge |first2=Jian |last3=Muterspaugh |first3=Matthew |last4=Singer |first4=Michael A |last5=Henry |first5=Gregory W |last6=González Hernández |first6=Jonay I |last7=Sithajan |first7=Sirinrat |last8=Jeram |first8=Sarik |last9=Williamson |first9=Michael |last10=Stassun |first10=Keivan |last11=Kimock |first11=Benjamin |last12=Varosi |first12=Frank |last13=Schofield |first13=Sidney |last14=Liu |first14=Jian |last15=Powell |first15=Scott |last16=Cassette |first16=Anthony |last17=Jakeman |first17=Hali |last18=Avner |first18=Louis |last19=Grieves |first19=Nolan |last20=Barnes |first20=Rory |last21=Zhao |first21=Bo |last22=Gilda |first22=Sankalp |last23=Grantham |first23=Jim |last24=Stafford |first24=Greg |last25=Savage |first25=David |last26=Bland |first26=Steve |last27=Ealey |first27=Brent |title=The first super-Earth detection from the high cadence and high radial velocity precision Dharma Planet Survey |journal=Monthly Notices of the Royal Astronomical Society |date=October 2018 |volume=480 |issue=2 |pages=2411–2422 |doi=10.1093/mnras/sty1933 |bibcode=2018MNRAS.480.2411M |arxiv=1807.07098 |s2cid=54871108 }}</ref><ref name=Rosenthal2021/>
and ] (26.2 ly, in 2021).<ref>{{cite journal |last1=Vedantham |first1=H. K. |last2=Callingham |first2=J. R. |last3=Shimwell |first3=T. W. |last4=Tasse |first4=C. |last5=Pope |first5=B. J. S. |last6=Bedell |first6=M. |last7=Snellen |first7=I. |last8=Best |first8=P. |last9=Hardcastle |first9=M. J. |last10=Haverkorn |first10=M. |last11=Mechev |first11=A. |last12=O’Sullivan |first12=S. P. |last13=Röttgering |first13=H. J. A. |last14=White |first14=G. J. |title=Coherent radio emission from a quiescent red dwarf indicative of star–planet interaction |journal=Nature Astronomy |date=June 2020 |volume=4 |issue=6 |pages=577–583 |doi=10.1038/s41550-020-1011-9 |arxiv=2002.08727 |bibcode=2020NatAs...4..577V |s2cid=211204712 }}</ref><ref>{{cite journal |last1=Mahadevan |first1=Suvrath |last2=Stefánsson |first2=Guðmundur |last3=Robertson |first3=Paul |last4=Terrien |first4=Ryan C. |last5=Ninan |first5=Joe P. |last6=Holcomb |first6=Rae J. |last7=Halverson |first7=Samuel |last8=Cochran |first8=William D. |last9=Kanodia |first9=Shubham |last10=Ramsey |first10=Lawrence W. |last11=Wolszczan |first11=Alexander |last12=Endl |first12=Michael |last13=Bender |first13=Chad F. |last14=Diddams |first14=Scott A. |last15=Fredrick |first15=Connor |last16=Hearty |first16=Fred |last17=Monson |first17=Andrew |last18=Metcalf |first18=Andrew J. |last19=Roy |first19=Arpita |last20=Schwab |first20=Christian |title=The Habitable-zone Planet Finder Detects a Terrestrial-mass Planet Candidate Closely Orbiting Gliese 1151: The Likely Source of Coherent Low-frequency Radio Emission from an Inactive Star |journal=The Astrophysical Journal Letters |date=3 February 2021 |volume=919 |issue=1 |pages=L9 |doi=10.3847/2041-8213/abe2b2 |arxiv=2102.02233 |bibcode=2021ApJ...919L...9M |s2cid=231802021 |doi-access=free }}</ref><ref name=Perger2021/>
There are also several instances where proposed exoplanets were later disproved by subsequent studies, including candidates around ] B (4.36 ly),<!--<ref>{{cite web |url=http://exoplanet.eu/catalog/alf_cen_b_b |title=alf Cen B b |publisher=Exoplanet.eu |website=The Extrasolar Planet Encyclopaedia |date=2011-05-27 |access-date=2014-05-17 |url-status=live |archive-url=https://web.archive.org/web/20140625075606/http://exoplanet.eu/catalog/alf_cen_b_b/ |archive-date=2014-06-25 }}</ref><ref>{{cite web |url=http://www.drewexmachina.com/2015/03/28/has-another-planet-been-found-orbiting-alpha-centauri-b/ |title=Has Another Planet Been Found Orbiting Alpha Centauri B? |first=Andrew |last=LePage |publisher=Drew Ex Machina |date=2015-03-28 |access-date=2015-09-17 |url-status=live |archive-url=https://web.archive.org/web/20150929103322/http://www.drewexmachina.com/2015/03/28/has-another-planet-been-found-orbiting-alpha-centauri-b/ |archive-date=2015-09-29 }}</ref>--><ref name="Rajpaul"/>
] (5.96 ly),<ref name=Ribas2018/><ref name=Lubin2021/> ] (5.96 ly),<ref name=Ribas2018/><ref name=Lubin2021/>
<!-- ] (6.59 ly, in 2013<ref>{{cite web|url=http://exoplanet.eu/catalog/luh_(ab)_b/ |work = The Extrasolar Planet Encyclopaedia| title= LUH (AB) b |publisher=Exoplanet.eu |date=2013-12-05 |access-date=2014-05-20}}</ref>), -->
] (12.8 ly),<ref name="BortleFausey2021"/> ] (12.8 ly),<ref name="BortleFausey2021"/>
] (14.1 ly),<ref name=nic/> ] (14.1 ly),<ref name=nic/>
] (15.9 ly),<ref>{{cite journal | display-authors=3 | title=Constraints on Long-period Planets from an L'- and M-band Survey of Nearby Sun-like Stars: Observations | last1=Heinze | first1=A. N. | last2=Hinz | first2=Philip M. | last3=Sivanandam | first3=Suresh | last4=Kenworthy | first4=Matthew | last5=Meyer | first5=Michael | last6=Miller | first6=Douglas | journal=The Astrophysical Journal | volume=714 | issue=2 | pages=1551&ndash;1569 |date=May 2010 | doi=10.1088/0004-637X/714/2/1551 | bibcode=2010ApJ...714.1551H |arxiv = 1003.5340 | s2cid=119199321 }}</ref> ] (15.9 ly),<ref>{{cite journal | display-authors=3 | title=Constraints on Long-period Planets from an L'- and M-band Survey of Nearby Sun-like Stars: Observations | last1=Heinze | first1=A. N. | last2=Hinz | first2=Philip M. | last3=Sivanandam | first3=Suresh | last4=Kenworthy | first4=Matthew | last5=Meyer | first5=Michael | last6=Miller | first6=Douglas | journal=The Astrophysical Journal | volume=714 | issue=2 | pages=1551&ndash;1569 |date=May 2010 | doi=10.1088/0004-637X/714/2/1551 | bibcode=2010ApJ...714.1551H |arxiv = 1003.5340 | s2cid=119199321 }}</ref>
] (16.2 ly),<ref name="GAPS2020"/> ] (16.2 ly),<ref name="GAPS2020"/>
] A (16.3 ly),<ref>{{cite journal |last1=Ma |first1=Bo |last2=Ge |first2=Jian |last3=Muterspaugh |first3=Matthew |last4=Singer |first4=Michael A |last5=Henry |first5=Gregory W |last6=González Hernández |first6=Jonay I |last7=Sithajan |first7=Sirinrat |last8=Jeram |first8=Sarik |last9=Williamson |first9=Michael |last10=Stassun |first10=Keivan |last11=Kimock |first11=Benjamin |last12=Varosi |first12=Frank |last13=Schofield |first13=Sidney |last14=Liu |first14=Jian |last15=Powell |first15=Scott |last16=Cassette |first16=Anthony |last17=Jakeman |first17=Hali |last18=Avner |first18=Louis |last19=Grieves |first19=Nolan |last20=Barnes |first20=Rory |last21=Zhao |first21=Bo |last22=Gilda |first22=Sankalp |last23=Grantham |first23=Jim |last24=Stafford |first24=Greg |last25=Savage |first25=David |last26=Bland |first26=Steve |last27=Ealey |first27=Brent |title=The first super-Earth detection from the high cadence and high radial velocity precision Dharma Planet Survey |journal=Monthly Notices of the Royal Astronomical Society |date=October 2018 |volume=480 |issue=2 |pages=2411–2422 |doi=10.1093/mnras/sty1933 |doi-access=free |bibcode=2018MNRAS.480.2411M |arxiv=1807.07098 |s2cid=54871108 }}</ref><ref name="Burrows2024"/>
] (19.3 ly),<ref>{{cite web |url=http://exoplanet.eu/catalog/vb_10_b/ |title=VB 10 b |website=The Extrasolar Planet Encyclopaedia |publisher=Exoplanet.eu |access-date=2015-09-17 |url-status=live |archive-url=https://web.archive.org/web/20150929194632/http://exoplanet.eu/catalog/vb_10_b/ |archive-date=2015-09-29 }}</ref> and ] (25.1 ly).<ref name="PNAS-20200420" />
] (19.3 ly),<ref>{{cite encyclopedia |url=https://exoplanet.eu/catalog/vb_10_b--550/ |title=VB 10 b |access-date=2015-09-17 |url-status=live |archive-url=https://web.archive.org/web/20150929194632/http://exoplanet.eu/catalog/vb_10_b/ |encyclopedia=] |archive-date=2015-09-29 }}</ref> and ] (25.1 ly).<ref name="PNAS-20200420" />


In 2021, a candidate planet was detected around ], though it has yet to be confirmed.<ref name="Hurt2021a"/> Another candidate planet, ], was directly imaged around ] A, though it may also be a clump of asteroids or an artifact of the discovery mechanism.<ref name="Wagner2021"/> In 2021, a candidate planet was detected around ], though it has yet to be confirmed.<ref name="Hurt2021a"/> Another candidate planet, ], was directly imaged around ] A, though it may also be a clump of asteroids or an artifact of the discovery mechanism.<ref name="Wagner2021"/> Candidate planets around {{Nowrap|]}} (8.77 ly)<ref name="GRAVITY2024">{{cite journal |last1=Abuter |first1=R. |last2=Amorim |first2=A. |last3=Benisty |first3=M. |last4=Berger |first4=J.-P. |last5=Bonnet |first5=H. |last6=Bourdarot |first6=G. |last7=Bourget |first7=P. |last8=Brandner |first8=W. |display-authors=1 |date=May 2024 |title=Astrometric detection of a Neptune-mass candidate planet in the nearest M-dwarf binary system GJ65 with VLTI/GRAVITY |journal=] |volume=685 |issue= |pages=L9 |arxiv=2404.08746 |bibcode=2024A&A...685L...9G |doi=10.1051/0004-6361/202449547 |collaboration=GRAVITY Collaboration}}</ref> and GJ 3378 (25.2 ly) were reported in 2024.<ref name="Moutou2024"/>


The Working Group on Extrasolar Planets of the International Astronomical Union adopted in 2003 a working definition on the upper limit for what constitutes a planet: not being massive enough to sustain thermonuclear fusion of ]. Some studies have calculated this to be somewhere around 13 times the ], and therefore objects more massive than this are usually classified as ]s.<ref name=IAU/> Some proposed candidate exoplanets have been shown to be massive enough to fall above the threshold, and thus are likely brown dwarfs, as is the case for: ] (13.1 ly),<ref>{{cite web |url=http://exoplanet.eu/catalog/scr_1845_b/ |title=SCR 1845 b |website=The Extrasolar Planet Encyclopaedia |publisher=Exoplanet.eu |date=2012-04-13 |access-date=2015-09-17 |url-status=live |archive-url=https://web.archive.org/web/20151001143712/http://exoplanet.eu/catalog/scr_1845_b/ |archive-date=2015-10-01 }}</ref> ] (30.3 ly),<ref>{{cite web |url=http://exoplanet.eu/catalog/sdss_141624_b/ |website=The Extrasolar Planet Encyclopaedia |title=SDSS 141624 b |publisher=Exoplanet.eu |date=2010-01-18 |access-date=2014-05-20 |url-status=dead |archive-url=https://web.archive.org/web/20140223211309/http://exoplanet.eu/catalog/sdss_141624_b/ |archive-date=2014-02-23 }}</ref> and ] (30 ly).<ref>{{cite web |url=http://exoplanet.eu/catalog/wise_1217+16_a_b/ |website=The Extrasolar Planet Encyclopaedia |title=WISE 1217+16A b |publisher=Exoplanet.eu |access-date=2014-05-17 |url-status=live |archive-url=https://web.archive.org/web/20170612172859/http://exoplanet.eu/catalog/wise_1217%2B16_a_b/ |archive-date=2017-06-12 }}</ref> The Working Group on Extrasolar Planets of the International Astronomical Union adopted in 2003 a working definition on the upper limit for what constitutes a planet: not being massive enough to sustain thermonuclear fusion of ]. Some studies have calculated this to be somewhere around 13 times the ], and therefore objects more massive than this are usually classified as ]s.<ref name=IAU/> Some proposed candidate exoplanets have been shown to be massive enough to fall above the threshold, and thus are likely brown dwarfs, as is the case for: ] (13.1 ly),<ref>{{cite encyclopedia |url=https://exoplanet.eu/catalog/scr_1845_b--321/ |title=SCR 1845 b |date=2012-04-13 |access-date=2015-09-17 |url-status=live |archive-url=https://web.archive.org/web/20151001143712/http://exoplanet.eu/catalog/scr_1845_b/ |encyclopedia=] |archive-date=2015-10-01 }}</ref> ] (30.3 ly),<ref>{{cite encyclopedia |url=http://exoplanet.eu/catalog/sdss_141624_b/ |title=SDSS 141624 b |date=2010-01-18 |access-date=2014-05-20 |url-status=dead |archive-url=https://web.archive.org/web/20140223211309/http://exoplanet.eu/catalog/sdss_141624_b/ |encyclopedia=] |archive-date=2014-02-23 }}</ref> and ] (30 ly).<ref>{{cite encyclopedia |url=https://exoplanet.eu/catalog/wise_1217_16_a_b--1465/ |title=WISE 1217+16A b |access-date=2014-05-17 |url-status=live |archive-url=https://web.archive.org/web/20170612172859/http://exoplanet.eu/catalog/wise_1217%2B16_a_b/ |encyclopedia=] |archive-date=2017-06-12 }}</ref>


Excluded from the current list are known examples of potential free-floating ]s, or "]s", which are bodies that are too small to undergo fusion yet they do not revolve around a star. Known such examples include: ] (7.4 ly),<ref name="NASA20140425"/> ], (13.4 ly)<ref name="Lucas2010"/> ] (18.6 ly),<ref name="Cushing2011"/> and ] (20.0 ly).<ref>{{Cite web | url=http://www.astronomy.com/news/2018/08/free-range-planet |title = Astronomers discover a nearby free-range planet with incredible magne}}</ref> Excluded from the current list are known examples of potential free-floating ]s, or "]s", which are bodies that are too small to undergo fusion yet they do not revolve around a star. Known such examples include: ] (7.4 ly),<ref name="NASA20140425"/> ], (13.4 ly)<ref name="Lucas2010"/> ] (18.6 ly),<ref name="Cushing2011"/> and ] (20.0 ly).<ref>{{Cite web | url=http://www.astronomy.com/news/2018/08/free-range-planet |title = Astronomers discover a nearby free-range planet with incredible magne| date=3 August 2018 }}</ref>


== See also == == See also ==
Line 541: Line 592:
* ] * ]
* ] * ]
* ]
* ]
* ] * ]
* ] * ]
Line 755: Line 804:
|last18=Reiners |first18=Ansgar |last18=Reiners |first18=Ansgar
|last19=Anglada-Escudé |first19=G. |last19=Anglada-Escudé |first19=G.
|date=2019-08-13 |title=Red Dots: A temperate 1.5 Earth-mass planet in a compact multi-terrestrial planet system around GJ1061 |doi=10.1093/mnras/staa248 |arxiv=1908.04717| s2cid=199551874 |language=en |bibcode=2020MNRAS.493..536D}}</ref> |date=2019-08-13 |title=Red Dots: A temperate 1.5 Earth-mass planet in a compact multi-terrestrial planet system around GJ1061 |volume=493 |issue=1 |page=536 |doi=10.1093/mnras/staa248 |doi-access=free |arxiv=1908.04717| s2cid=199551874 |language=en |bibcode=2020MNRAS.493..536D}}</ref>


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<ref name=Perger2021>{{citation|arxiv=2103.10216|year=2021|title=The CARMENES search for exoplanets around M dwarfs, No evidence for a super-Earth in a 2-day orbit around GJ 1151|doi=10.1051/0004-6361/202140786|last1=Perger|first1=M.|last2=Ribas|first2=I.|last3=Anglada-Escudé|first3=G.|last4=Morales|first4=J. C.|last5=Amado|first5=P. J.|last6=Caballero|first6=J. A.|last7=Quirrenbach|first7=A.|last8=Reiners|first8=A.|last9=Béjar|first9=V. J. S.|last10=Dreizler|first10=S.|last11=Galadí-Enríquez|first11=D.|last12=Hatzes|first12=A. P.|last13=Henning|first13=Th.|last14=Jeffers|first14=S. V.|last15=Kaminski|first15=A.|last16=Kürster|first16=M.|last17=Lafarga|first17=M.|last18=Montes|first18=D.|last19=Pallé|first19=E.|last20=Rodríguez-López|first20=C.|last21=Schweitzer|first21=A.|last22=Zapatero Osorio|first22=M. R.|last23=Zechmeister|first23=M.|journal=Astronomy & Astrophysics|volume=649|pages=L12|bibcode=2021A&A...649L..12P|s2cid=126038821}}</ref> <ref name=Perger2021>{{citation|arxiv=2103.10216|year=2021|title=The CARMENES search for exoplanets around M dwarfs, No evidence for a super-Earth in a 2-day orbit around GJ 1151|doi=10.1051/0004-6361/202140786|last1=Perger|first1=M.|last2=Ribas|first2=I.|last3=Anglada-Escudé|first3=G.|last4=Morales|first4=J. C.|last5=Amado|first5=P. J.|last6=Caballero|first6=J. A.|last7=Quirrenbach|first7=A.|last8=Reiners|first8=A.|last9=Béjar|first9=V. J. S.|last10=Dreizler|first10=S.|last11=Galadí-Enríquez|first11=D.|last12=Hatzes|first12=A. P.|last13=Henning|first13=Th.|last14=Jeffers|first14=S. V.|last15=Kaminski|first15=A.|last16=Kürster|first16=M.|last17=Lafarga|first17=M.|last18=Montes|first18=D.|last19=Pallé|first19=E.|last20=Rodríguez-López|first20=C.|last21=Schweitzer|first21=A.|last22=Zapatero Osorio|first22=M. R.|last23=Zechmeister|first23=M.|journal=Astronomy & Astrophysics|volume=649|pages=L12|bibcode=2021A&A...649L..12P|s2cid=126038821}}</ref>


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}} }}

Latest revision as of 17:40, 27 November 2024

Epsilon Indi Ab, 12 light-years away, with its parent star Epsilon Indi A blacked out, as pictured by JWST in 2023.
Distribution of nearest known exoplanets as of March 2018

There are 7,026 known exoplanets, or planets outside the Solar System that orbit a star, as of July 24, 2024; only a small fraction of these are located in the vicinity of the Solar System. Within 10 parsecs (32.6 light-years), there are 106 exoplanets listed as confirmed by the NASA Exoplanet Archive. Among the over 500 known stars and brown dwarfs within 10 parsecs, around 60 have been confirmed to have planetary systems; 51 stars in this range are visible to the naked eye, eight of which have planetary systems.

The first report of an exoplanet within this range was in 1998 for a planet orbiting around Gliese 876 (15.3 light-years (ly) away), and the latest as of 2024 is one around Struve 2398 A (11.5 ly). The closest exoplanets are those found orbiting the star closest to the Solar System, which is Proxima Centauri 4.25 light-years away. The first confirmed exoplanet discovered in the Proxima Centauri system was Proxima Centauri b, in 2016. HD 219134 (21.6 ly) has six exoplanets, the highest number discovered for any star within this range.

Most known nearby exoplanets orbit close to their stars. A majority are significantly larger than Earth, but a few have similar masses, including planets around YZ Ceti, Gliese 367, Proxima Centauri, and Barnard's Star which may be less massive than Earth. Several confirmed exoplanets are hypothesized to be potentially habitable, with Proxima Centauri b and GJ 1002 b (15.8 ly) considered among the most likely candidates. The International Astronomical Union has assigned proper names to some known extrasolar bodies, including nearby exoplanets, through the NameExoWorlds project. Planets named in the 2015 event include the planets around Epsilon Eridani (10.5 ly) and Fomalhaut, while planets named in the 2022 event include those around Gliese 436, Gliese 486, and Gliese 367.

Exoplanets within 10 parsecs

Key to colors
Mercury, Earth and Jupiter (for comparison purposes)
Confirmed multiplanetary systems
Exoplanets believed to be potentially habitable
Confirmed exoplanets
Host star system Companion exoplanet (in order from star) Notes and additional planetary observations
Name Distance
(ly)
Apparent
magnitude
(V) 		Mass
(M☉)
Label
 Mass
(ME)
 		Radius
(R🜨)
Semi-major axis
(AU)
Orbital period
(days)
Eccentricity
Inclination
(°)
Discovery
method 		Discovery year
Sun 0.000016 −26.7 1 Mercury 0.055 0.3829 0.387 88.0 0.205 — — — —
Earth 1 1 1 365.3 0.0167 — — —
Jupiter 317.8 10.973 5.20 4,333 0.0488 — — —
Proxima Centauri 4.2465 11.13 0.123 d ≥0.26 — 0.0289 5.122 0.04 — RV 2022 one disputed candidate (c)
b ≥1.07 — 0.0486 11.19 0.02 — RV 2016
Barnard's Star 5.9629 9.51 0.162 b ≥0.37 — 0.0229 3.153 0.16 — RV 2024
Lalande 21185 8.304 7.52 0.46 b ≥2.69 — 0.0788 12.94 0.06 — RV 2019 1 candidate
c ≥13.6 — 2.94 2,946 0.13 — RV 2021
Epsilon Eridani 10.489 3.73 0.781 Ægir 242 — 3.53 2,689 0.26 166.5 RV 2000 1 inferred planet, 1 or possibly 2 inner debris discs, and an outer disc
Lacaille 9352 10.724 7.34 0.489 b ≥4.2 — 0.068 9.262 0.03 — RV 2019 1 candidate
c ≥7.6 — 0.120 21.79 0.03 — RV 2019
Ross 128 11.007 11.1 0.168 b ≥1.40 — 0.0496 9.866 0.12 — RV 2017
Gliese 725 A 11.491 8.94 0.330 b ≥2.78 — 0.068 11.2201 0.0 — RV 2024
Groombridge 34 A 11.619 8.1 0.38 b ≥3.03 — 0.072 11.44 0.09 ~54? RV 2014
c ≥36 — 5.4 7,600 0.27 ~54? RV 2018
Epsilon Indi A 11.867 4.83 0.762 b 2005 — 28.4 63,400 0.40 103.7 RV 2018 nearest exoplanet directly imaged
Tau Ceti 11.912 3.50 0.78 g ≥1.75 — 0.133 20.0 0.06 ~35? RV 2017 4 disputed candidates
h ≥1.8 — 0.243 49.4 0.23 ~35? RV 2017
e ≥3.9 — 0.538 163 0.18 ~35? RV 2017
f ≥3.9 — 1.33 640 0.16 ~35? RV 2017
GJ 1061 11.984 7.52 0.113 b ≥1.37 — 0.021 3.204 <0.31 — RV 2019 two solutions for d's orbit
c ≥1.74 — 0.035 6.689 <0.29 — RV 2019
d ≥1.64 — 0.054 13.03 <0.53 — RV 2019
YZ Ceti 12.122 12.1 0.130 b ≥0.70 — 0.0163 2.021 0.06 — RV 2017
c ≥1.14 — 0.0216 3.060 0.0 — RV 2017
d ≥1.09 — 0.0285 4.656 0.07 — RV 2017
Luyten's Star 12.348 11.94 0.29 c ≥1.18 — 0.0365 4.723 0.10 — RV 2017
b ≥2.89 — 0.0911 18.65 0.17 — RV 2017
d ≥10.8 — 0.712 414 0.17 — RV 2019
e ≥9.3 — 0.849 542 0.03 — RV 2019
Teegarden's Star 12.497 15.40 0.08 b ≥1.16 — 0.0259 4.906 0.03 — RV 2019
c ≥1.05 — 0.0455 11.42 0.04 — RV 2019
d ≥0.82 — 0.0791 26.13 0.07 — RV 2024
Wolf 1061 14.050 10.1 0.25 b ≥1.91 — 0.0375 4.887 0.15 — RV 2015
c ≥3.41 — 0.0890 17.87 0.11 — RV 2015
d ≥7.7 — 0.470 217 0.55 — RV 2015
TZ Arietis 14.578 12.30 0.14 b ≥67 — 0.88 771 0.46 — RV 2019 2 refuted candidates
Gliese 687 14.839 9.15 0.41 b ≥17.2 — 0.163 38.14 0.17 — RV 2014
c ≥16.0 — 1.165 728 0.40 — RV 2019
Gliese 674 14.849 9.38 0.35 b ≥11.1 — 0.039 4.694 0.20 — RV 2007
Gliese 876 15.238 10.2 0.33 d 6.68 — 0.0210 1.938 0.04 56.7 RV 2005
c 235 — 0.1309 30.10 0.26 56.7 RV 2000
b 749 — 0.2098 61.10 0.03 56.7 RV 1998
e 16 — 0.3355 123.6 0.05 56.7 RV 2010
GJ 1002 15.806 13.84 0.12 b ≥1.08 — 0.0457 10.35 — — RV 2022
c ≥1.36 — 0.0738 21.2 — — RV 2022
Gliese 832 16.200 8.67 0.45 b 315 — 3.7 3,853 0.05 51 or 134 RV 2008 1 refuted candidate
GJ 3323 17.531 12.2 0.164 b ≥2.0 — 0.0328 5.36 0.2 — RV 2017
c ≥2.3 — 0.126 40.5 0.2 — RV 2017
Gliese 251 18.215 9.65 0.372 b ≥4.0 — 0.0818 14.2 0.10 — RV 2020
Gliese 229 A 18.791 8.14 0.58 c ≥7.3 — 0.339 122 0.19 — RV 2020 Ab not confirmed until 2020
b ≥8.5 — 0.898 526 0.10 — RV 2014
Gliese 752 A 19.292 9.13 0.46 b ≥12.2 — 0.343 106 0.10 — RV 2018
82 G. Eridani 19.704 4.26 0.85 b ≥2.0 — 0.13 18.3 0.09 — RV 2011 5 disputed candidates
d ≥4.7 — 0.37 89.6 0.13 — RV 2011
Gliese 555 20.395 11.32 0.29 b ≥5.5 — 0.142 36.1 0.08 — RV 2023 1 candidate
EQ Pegasi A 20.400 10.38 0.436 b 718 — 0.643 284 0.35 69.2 Astrometry 2022
Gliese 581 20.549 10.5 0.295 e 2.5 — 0.0280 3.15 0.01 47 RV 2009 3 refuted candidates and a disc
b 20.5 — 0.0399 5.37 0.03 47 RV 2005
c 6.8 — 0.0718 12.9 0.03 47 RV 2007
Gliese 338 B 20.658 7.0 0.64 b ≥10.3 — 0.141 24.5 0.11 — RV 2020
Gliese 625 21.131 10.2 0.30 b ≥2.8 — 0.0784 14.6 ~0.1 — RV 2017
HD 219134 21.336 5.57 0.78 b 4.7 1.60 0.0388 3.09 ~0 85.05 RV 2015
c 4.4 1.51 0.065 6.77 0.062 87.28 RV 2015
d ≥16 — 0.237 46.9 0.138 ~87? RV 2015
f ≥7.3 — 0.146 22.7 0.148 ~87? RV 2015
g ≥11 — 0.375 94.2 0 ~87? RV 2015
h (e) ≥108 — 3.11 2,247 0.06 ~87? RV 2015
LTT 1445 A 22.387 10.53 0.26 c 1.54 1.15 0.0266 3.12 <0.22 87.43 Transit 2021 1 candidate
b 2.87 1.30 0.0381 5.36 <0.11 89.68 Transit 2019
Gliese 393 22.953 8.65 0.41 b ≥1.71 — 0.0540 7.03 0.00 — RV 2019
Gliese 667 C 23.623 10.2 0.33 b ≥5.4 — 0.049 7.20 0.13 ~52? RV 2009 5 dubious candidates
c ≥3.9 — 0.1251 28.2 0.03 ~52? RV 2011
Gliese 514 24.878 9.03 0.53 b ≥5.2 — 0.421 140 0.45 — RV 2022
GJ 1151 26.231 14.01 0.164 c ≥10.6 — 0.571 390 — — RV 2023 1 refuted candidate
Gliese 486 26.351 11.395 0.32 Su 2.8 1.31 0.0173 1.47 <0.05 88.4 Transit 2021
Gliese 686 26.613 9.58 0.42 b ≥7.1 — 0.097 15.5 0.04 — RV 2019
GJ 1289 27.275 12.67 0.21 b ≥6.3 — 0.27 112 0 — RV 2024
61 Virginis 27.836 4.74 0.95 b ≥6.1 — 0.05 4.22 0.05 ~77? RV 2009 a debris disc
c ≥17.9 — 0.22 38.1 0.06 ~77? RV 2009
d ≥10.5 — 0.47 123 0.12 ~77? RV 2009
CD Ceti 28.052 14.001 0.161 b ≥3.95 — 0.0185 2.29 0 — RV 2020
Gliese 785 28.739 6.13 0.78 b ≥17 — 0.32 75 0.13 — RV 2010
c ≥24 — 1.18 530 ~0.3 — RV 2011
Gliese 849 28.750 10.4 0.49 b ≥270 — 2.26 1,910 0.05 — RV 2006
c ≥300 — 4.82 5,520 0.087 — RV 2006
Gliese 433 29.605 9.79 0.48 b ≥6.0 — 0.062 7.37 0.04 — RV 2009
d ≥5.2 — 0.178 36.1 0.07 — RV 2020
c ≥32 — 4.82 5,090 0.12 — RV 2012
HD 102365 A 30.396 4.89 0.85 b ≥16 — 0.46 122 0.34 — RV 2010
Gliese 367 30.719 9.98 0.45 Tahay 0.63 0.70 0.0071 0.322 0.06 79.89 Transit 2021
c ≥4.1 — 0.077 11.5 0.09 ~80? RV 2023
d ≥6.0 — 0.159 34.4 0.14 ~80? RV 2023
Gliese 357 30.776 10.9 0.34 b 6.1 1.17 0.035 3.93 0.02 88.92 Transit 2019
c ≥3.6 — 0.061 9.13 0.04 ~89? RV 2019
d ≥7.7 — 0.204 55.7 0.03 ~89? RV 2019
Gliese 176 30.937 10.1 0.45 b ≥8.0 — 0.066 8.77 0.08 — RV 2007 1 disputed candidate
GJ 3512 30.976 13.11 0.123 b ≥147 — 0.338 204 0.44 — RV 2019
c ≥54 — >1.2 >1390 — — RV 2019
Wolf 1069 31.229 13.99 0.167 b ≥1.26 — 0.0672 15.6 — — RV 2023
AU Microscopii 31.683 8.63 0.50 b 17 4.38 0.0645 8.463 0.10 89.03 Transit 2020 2 candidates
c <28 3.51 0.1101 18.86 0 88.62 Transit 2020
Gliese 436 31.882 10.67 0.41 Awohali 21.4 4.33 0.0280 2.64 0.15 85.8 RV 2004
Gliese 49 32.158 8.9 0.57 b ≥16.4 — 0.106 17.3 0.03 — RV 2019
GJ 3988 32.316 13.6 0.184 b ≥3.7 — 0.0405 6.944 0 — RV 2023
HD 260655 32.608 9.77 0.439 b 2.14 1.240 0.0293 2.780 0.039 87.35 Transit 2022
c 3.09 1.533 0.0475 5.706 0.038 87.79 Transit 2022

Excluded objects

Unlike for bodies within the Solar System, there is no clearly established method for officially recognizing an exoplanet. According to the International Astronomical Union, an exoplanet should be considered confirmed if it has not been disputed for five years after its discovery. There have been examples where the existence of exoplanets has been proposed, but even after follow-up studies their existence is still considered doubtful by some astronomers. Such cases include Wolf 359 (7.9 ly, in 2019), LHS 288 (15.8 ly, in 2007), and Gliese 682 (16.3 ly, in 2014). There are also several instances where proposed exoplanets were later disproved by subsequent studies, including candidates around Alpha Centauri B (4.36 ly), Barnard's Star (5.96 ly), Kapteyn's Star (12.8 ly), Van Maanen 2 (14.1 ly), Groombridge 1618 (15.9 ly), AD Leonis (16.2 ly), 40 Eridani A (16.3 ly), VB 10 (19.3 ly), and Fomalhaut (25.1 ly).

In 2021, a candidate planet was detected around Vega, though it has yet to be confirmed. Another candidate planet, Candidate 1, was directly imaged around Alpha Centauri A, though it may also be a clump of asteroids or an artifact of the discovery mechanism. Candidate planets around Luyten 726-8 (8.77 ly) and GJ 3378 (25.2 ly) were reported in 2024.

The Working Group on Extrasolar Planets of the International Astronomical Union adopted in 2003 a working definition on the upper limit for what constitutes a planet: not being massive enough to sustain thermonuclear fusion of deuterium. Some studies have calculated this to be somewhere around 13 times the mass of Jupiter, and therefore objects more massive than this are usually classified as brown dwarfs. Some proposed candidate exoplanets have been shown to be massive enough to fall above the threshold, and thus are likely brown dwarfs, as is the case for: SCR 1845-6357 B (13.1 ly), SDSS J1416+1348 B (30.3 ly), and WISE 1217+1626 B (30 ly).

Excluded from the current list are known examples of potential free-floating sub-brown dwarfs, or "rogue planets", which are bodies that are too small to undergo fusion yet they do not revolve around a star. Known such examples include: WISE 0855−0714 (7.4 ly), UGPS 0722-05, (13.4 ly) WISE 1541−2250 (18.6 ly), and SIMP J01365663+0933473 (20.0 ly).

See also

Notes

  1. Listed values are primarily taken from NASA Exoplanet Archive, but other databases include a few additional exoplanet entries tagged as "Confirmed" that have yet to be compiled into the NASA archive. Such databases include:
    "Exoplanet Catalog". Extrasolar Planets Encyclopaedia. 1995. Full table.
    "Exoplanets Data Explorer". Exoplanet Orbit Database. California Planet Survey. Click the "+" button to visualize additional parameters.
    "Open Exoplanet Catalogue". Click the "Show options" to visualize additional parameters. Archived from the original on 2017-09-02. Retrieved 2015-02-14.
  2. For reference, the 100th closest known star system in April 2021 was EQ Pegasi (20.4 ly).
  3. According to the Bortle scale, an astronomical object is visible to the naked eye under "typical" dark-sky conditions in a rural area if it has an apparent magnitude smaller than +6.5. To the unaided eye, the limiting magnitude is +7.6 to +8.0 under "excellent" dark-sky conditions (with effort).
  4. The star Epsilon Eridani was named Ran (after Rán, the Norse goddess of the sea), and the planet Epsilon Eridani b was named AEgir (after Ægir, Rán's husband), while the planet Fomalhaut b was named Dagon (after Dagon, an ancient Syrian “fish god”).
  5. Exoplanet naming convention assigns uncapitalized letters starting from b to each planet based on chronological order of their initial report, and in increasing order of distance from the parent star for planets reported at the same time. Omitted letters signify planets that have yet to be confirmed, or planets that have been retracted altogether.
  6. Most reported exoplanet masses have very large error margins (typically, between 10% and 30%). The mass of an exoplanet has generally been inferred from measurements on changes in the radial velocity of the host star, but this kind of measurement only allows for an estimate on the exoplanet's orbital parameters, but not on their orbital inclination (i). As such, most exoplanets only have an estimated minimum mass (Mreal*sin(i)), where their true masses are statistically expected to come close to this minimum, with only about 13% chance for the mass of an exoplanet to be more than double its minimum mass.

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