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list of exomoon candidates

{{short description|None}}

{{as of|2025}}, there have been no positive confirmations of satellites of extra-solar planets (exomoons); however, some evidence in favour of their existence has been produced.

Timeline

{{dynamic list}}

  • {{date table sorting|2012| | }} — It has been surmised that J1407b, a possibly planetary-mass object that eclipsed the star V1400 Centauri (aka. J1407) in 2007, may have a few moons based on gaps observed in its circumstellar disk or ring system.{{cite web |url=https://www.sciencedaily.com/releases/2012/01/120109115830.htm |title=Saturn-like ring system eclipses Sun-like star |access-date=9 March 2018 |url-status=live |archive-url=https://web.archive.org/web/20160919150711/https://www.sciencedaily.com/releases/2012/01/120109115830.htm |archive-date=19 September 2016 |quotation="Mamajek thinks his team could be either observing the late stages of planet formation if the transiting object is a star or brown dwarf, or possibly moon formation if the transiting object is a giant planet"}} Later studies have since found that J1407b is most likely a free-floating sub-brown dwarf or rogue planet, possibly less than 6 Jupiter masses.
  • {{date table sorting|2012| | }} — The confirmed hot Jupiter planet WASP-12b may also possess a moon.[http://www.ria.ru/science/20120206/558647431.html Российские астрономы впервые открыли луну возле экзопланеты] {{webarchive|url=https://web.archive.org/web/20120310222322/http://www.ria.ru/science/20120206/558647431.html |date=10 March 2012 }} (in Russian) – "Studying of a curve of change of shine of WASP-12b has brought to the Russian astronomers unusual result: regular splashes were found out.<...> Though stains on a star surface also can cause similar changes of shine, observable splashes are very similar on duration, a profile and amplitude that testifies for benefit of exomoon existence."
  • {{date table sorting|2013|12| }}, {{date table sorting|2014|04| }} — A candidate exomoon of a free-floating planet MOA-2011-BLG-262L, was announced, but due to degeneracies in the modelling of the microlensing event, the observations can also be explained as a Neptune-mass planet orbiting a low-mass red dwarf, a scenario the authors consider to be more likely.{{cite journal |author=Bennett, D.P. |display-authors=etal |title=A Sub-Earth-Mass Moon Orbiting a Gas Giant Primary or a High Velocity Planetary System in the Galactic Bulge |journal= The Astrophysical Journal|arxiv=1312.3951 |bibcode = 2014ApJ...785..155B |doi = 10.1088/0004-637X/785/2/155 |volume=785 |issue=2 |pages=155|year=2014 |s2cid=118327512 }}{{cite web |last=Clavin |first=Whitney |title=Faraway Moon or Faint Star? Possible Exomoon Found |url=http://www.jpl.nasa.gov/news/news.php?release=2014-109 |date=10 April 2014 |work=NASA |access-date=10 April 2014 |url-status=live |archive-url=https://web.archive.org/web/20140412095852/http://www.jpl.nasa.gov/news/news.php?release=2014-109 |archive-date=12 April 2014 }}{{cite web|url=https://www.newscientist.com/article/dn24773-first-exomoon-glimpsed--1800-light-years-from-earth.html|title=First exomoon glimpsed – 1800 light years from Earth|publisher=New Scientist|access-date=20 December 2013|url-status=live|archive-url=https://web.archive.org/web/20131220020356/http://www.newscientist.com/article/dn24773-first-exomoon-glimpsed--1800-light-years-from-earth.html|archive-date=20 December 2013}} In 2024 the latter scenario was confirmed.
  • {{date table sorting|2018|10| }} — researchers using the Hubble Space Telescope published observations of the candidate exomoon Kepler-1625b I, which suggest that the host planet is likely several Jupiter masses, while the exomoon may have a mass and radius similar to Neptune. The study concluded that the exomoon hypothesis is the simplest and best explanation for the available observations, though warned that it is difficult to assign a precise probability to its existence and nature.{{cite journal | title=HEK VI: On the Dearth of Galilean Analogs in Kepler and the Exomoon Candidate Kepler-1625b I | last1=Teachey | first1=Alex | last2=Kipping | first2=David M. | last3=Schmitt | first3=Allan R. | display-authors=1 | journal=The Astronomical Journal | volume=155 | issue=1 | at=36 | year=2017 | arxiv=1707.08563 | bibcode=2018AJ....155...36T | doi=10.3847/1538-3881/aa93f2 | s2cid=118911978 | doi-access=free }}{{cite journal | title=Evidence for a large exomoon orbiting Kepler-1625b | last1=Teachey | first1=Alex | last2=Kipping | first2=David M. | journal= Science Advances | volume=4 | issue=10 | pages=eaav1784 |date=4 October 2018 | doi=10.1126/sciadv.aav1784 | pmid=30306135 | pmc=6170104 | bibcode=2018SciA....4.1784T | arxiv=1810.02362 }}
  • {{date table sorting|2019|04| }} — reanalysis concluded that the data was fit better by a planet-only model. According to this study, the discrepancy was an artifact of the data reduction, and Kepler-1625b I likely does not exist.{{cite journal |title=No Evidence for Lunar Transit in New Analysis of HST Observations of the Kepler-1625 System|author1=Laura Kreidberg|author2=Rodrigo Luger|author3=Megan Bedell|journal=The Astrophysical Journal |date=24 April 2019|volume=877 |issue=2 |doi=10.3847/2041-8213/ab20c8|arxiv=1904.10618|s2cid=129945202 |doi-access=free |bibcode=2019ApJ...877L..15K }}
  • {{date table sorting|2019|09| }} – A hypothesis involving potential transits of large exomoons being detached from their planets (see ploonet) was posited to explain the light flux-variations of the Tabby's Star, which were identified from the data collected by Kepler space telescope.{{cite journal |title=Ploonets: formation, evolution, and detectability of tidally detached exomoons |journal=Monthly Notices of the Royal Astronomical Society |first1=Mario |last1=Sucerquia |first2=Jaime A. |last2=Alvarado-Montes |first3=Jorge I. |last3=Zuluaga |first4=Nicolás |last4=Cuello |first5=Cristian |last5=Giuppone |display-authors=1 |volume=489 |issue=2 |pages=2313–2322 |date=October 2019 |doi=10.1093/mnras/stz2110 |doi-access=free |bibcode=2019MNRAS.489.2313S |arxiv=1906.11400 |s2cid=195700030}}
  • {{date table sorting|2020|08| }} — A paper by Chris Fox and Paul Wiegert examined the Kepler dataset for indications of exomoons solely from transit timing variations. Eight candidate signals were found that were consistent with an exomoon, however the signals could also be explained by the presence of another planet. Fox and Wiegert's conclusion was more and higher quality transit timing data would be required to establish whether these are truly moons or not.{{cite journal |last1=Fox |first1=Chris |last2=Wiegert |first2=Paul |arxiv=2006.12997 |title=Exomoon Candidates from Transit Timing Variations: Eight Kepler systems with TTVs explainable by photometrically unseen exomoons |journal=Monthly Notices of the Royal Astronomical Society |date=23 November 2020 |volume=501 |issue=2 |pages=2378–2393 |doi=10.1093/mnras/staa3743 |doi-access=free |bibcode=2021MNRAS.501.2378F |s2cid=219980961 }} David Kipping re-derived the timings of six of the eight targets (based on a pre-peer review version) and evaluated the TTV evidence as uncompelling. The same study finds that Kepler-1625b I remains an exomoon candidate.{{cite journal |last1=Kipping |first1=David |arxiv=2008.03613 |title=An Independent Analysis of the Six Recently Claimed Exomoon Candidates |journal=The Astrophysical Journal |date=8 August 2020|volume=900 |issue=2 |pages=L44 |doi=10.3847/2041-8213/abafa9 |bibcode=2020ApJ...900L..44K |s2cid=225253170 |doi-access=free }}
  • {{date table sorting|2021|08| }} — astronomers reported an habitable-zone 1.7 {{Earth radius}} exomoon candidate transiting one of the components in the planetary-mass binary 2MASS J1119-1137AB.{{cite journal|last1=Limbach|first1=Mary Anne|last2=Vos|first2=Johanna M.|last3=Winn|first3=Joshua N.|last4=Heller|first4=Rene|last5=Mason|first5=Jeffrey C.|last6=Schneider|first6=Adam C.|last7=Dai|first7=Fei|date=2021-08-18|title=On the Detection of Exomoons Transiting Isolated Planetary-mass Objects|journal=The Astrophysical Journal Letters|volume=918|issue=2|pages=L25|doi=10.3847/2041-8213/ac1e2d|arxiv=2108.08323|bibcode=2021ApJ...918L..25L|s2cid=237213523|language=en |doi-access=free }}
  • {{date table sorting|2022|01| }} — an exomoon candidate was reported around the planet Kepler-1708b, and because it is orbiting a planet at approximately 1.6 AU from a star that is slightly more luminous than the Sun, it too could be within the habitable zone.{{cite journal |last1=Kipping |first1=David |last2=Bryson |first2=Steve |display-authors=etal |date=13 January 2022 |title=An exomoon survey of 70 cool giant exoplanets and the new candidate Kepler-1708 b-i |journal=Nature |volume= 6|issue= 3|pages= 367–380|doi= 10.1038/s41550-021-01539-1|pmid=35399159 |pmc=8938273 |arxiv=2201.04643 |bibcode=2022NatAs...6..367K}} However, this candidate is based on limited observations (only two transits) and some consider the data to be non-convincing.{{cite web |title=Astronomers may have found a huge moon around a Jupiter-like exoplanet |url=https://www.newscientist.com/article/2304546-astronomers-may-have-found-a-huge-moon-around-a-jupiter-like-exoplanet/ |website=New Scientist |access-date=28 January 2022}}
  • {{date table sorting|2022|11| }} — another exomoon candidate was reported around the planet Kepler-1513b (KOI-3678.01). Unlike the previous giant exomoon candidates of Kepler-1625 and Kepler-1708, this exomoon would be terrestrial-mass, ranging from 0.76 Lunar masses to 0.34 Earth masses depending on the planet's mass and moon's orbital period.{{cite journal |last1=Kipping |first1=David |last2=Yahalomi |first2=Daniel A. |date=January 2023 |title=A search for transit timing variations within the exomoon corridor using Kepler data |journal=Monthly Notices of the Royal Astronomical Society |volume=518 |issue=3 |pages=3482–3493 |doi=10.1093/mnras/stac3360 |doi-access=free |arxiv=2211.06210 |bibcode=2023MNRAS.518.3482K}}
  • {{date table sorting|2023|10| }} — a follow-up study by the same team found that the observed TTVs are caused by a second planet in the system, and not by a moon.{{cite journal |last1=Yahalomi |first1=Daniel A. |last2=Kipping |first2=David |display-authors=etal |date=January 2024 |title=Not So Fast Kepler-1513: A Perturbing Planetary Interloper in the Exomoon Corridor |journal=Monthly Notices of the Royal Astronomical Society |volume=527 |issue=1 |pages=620–639 |doi=10.1093/mnras/stad3070 |doi-access=free |arxiv=2310.03802 |bibcode=2024MNRAS.527..620Y}}
  • {{date table sorting|2023|12| }} — The exomoon candidate around Kepler-1625b was again challenged, along with the Kepler-1708b candidate. This study argues that the statistical significance of these exomoon candidates is lower than previously claimed (with false positive probabilities of 10.9% and 1.6%, respectively) and that true giant exomoons would have stronger evidence. Evidence for exomoon transits may be caused by stellar activity in the Kepler light curves.{{cite journal |last1=Heller |first1=René |last2=Hippke |first2=Michael |date=December 2023 |title=Large exomoons unlikely around Kepler-1625 b and Kepler-1708 b |journal=Nature Astronomy |volume= 8|issue= 2|pages= 193–206|doi=10.1038/s41550-023-02148-w |arxiv=2312.03786 |bibcode=2024NatAs...8..193H}} Kipping's team published a response arguing that these exomoon candidates remain possible.{{cite journal |last1=Kipping |first1=David |last2=Teachey |first2=Alex |date=January 2024 |title=A Reply to: Large Exomoons unlikely around Kepler-1625 b and Kepler-1708 b |journal=Nature Astronomy |volume= |issue= |pages= |doi= |arxiv=2401.10333}}
  • {{date table sorting|2024|10| }} — New measurements with the Very Large Telescope of the star WASP-49 gave more evidences favoring the presence of a possible volcanically active-moon around the hot Jupiter WASP-49b.{{Cite journal |last1=Oza |first1=Apurva V. |last2=Seidel |first2=Julia V. |last3=Hoeijmakers |first3=H. Jens |last4=Unni |first4=Athira |last5=Kesseli |first5=Aurora Y. |last6=Schmidt |first6=Carl A. |last7=Sivarani |first7=Thirupathi |last8=Bello-Arufe |first8=Aaron |last9=Gebek |first9=Andrea |last10=Meyer zu Westram |first10=Moritz |last11=Sousa |first11=Sérgio G. |last12=Lopes |first12=Rosaly M. C. |last13=Hu |first13=Renyu |last14=de Kleer |first14=Katherine |last15=Fisher |first15=Chloe |date=2024-10-01 |title=Redshifted Sodium Transient near Exoplanet Transit |journal=The Astrophysical Journal Letters |volume=973 |issue=2 |pages=L53 |doi=10.3847/2041-8213/ad6b29 |doi-access=free |arxiv=2409.19844 |bibcode=2024ApJ...973L..53O |issn=2041-8205}}

Table

class="wikitable sortable"

! Host star
of the
host planet(s)

! Planet designation

! Planet mass

! Planet
semimajor
axis (AU)

! Exomoon
semimajor
axis

! Exomoon
mass ({{Earth mass|sym=y|link=yes}})

! Notes

N/A

| J1407b

| {{sort|06|<6}} {{Jupiter mass|link=yes}}

| N/A

| 0.396–0.421 AU

| <0.8

| One possible exomoon residing in a 4 million km-wide gap in J1407b's circumplanetary disk. Other ring gaps in J1407b's disk may also contain exomoons.

Beta Pictoris

|Beta Pictoris b

|9.3{{±|2.6|2.5}} {{Jupiter mass}}

|10.26

|0.03 to 0.05 AU

|≳15

|Found via the predicted misaligment of the planet's obliquity, which is yet to be confirmed by JWST observations but is currently likely.{{Cite journal |arxiv=2412.05988 |first1=Michael |last1=Poon |first2=Hanno |last2=Rein |title=A potential exomoon from the predicted planet obliquity of β Pictoris b |date=2024-12-08 |last3=Pham |first3=Dang|journal=The Open Journal of Astrophysics |volume=7 |doi=10.33232/001c.127130 }}

N/A

|2MASS J1119-1137A or B

|3.7 {{Jupiter mass|link=yes}}

|3.6 ± 0.9
separation from each other

|0.004 - 0.009 AU

|0.5 - 1

|Found using the transit method. A habitable-zone exomoon candidate transiting a directly imaged free-floating planet or isolated planetary-mass object.

N/A

|2MASS J2117-2940

|7 {{Jupiter mass|link=yes}}

|N/A

|0.005 AU

|~0.5

|Candidate exomoon transit detected in Spitzer observations of 2MASS J21171431-2940034.{{cite arXiv |last1=Limbach |first1=Mary Anne |title=Occurrence Rates of Exosatellites Orbiting 3-30M$_{\rm Jup}$ Hosts from 44 Spitzer Light Curves |date=2024-05-13 |eprint=2405.08116 |last2=Vos |first2=Johanna M. |last3=Vanderburg |first3=Andrew |last4=Dai |first4=Fei|class=astro-ph.EP }}

DH TauriDH Tauri b10.6 {{Jupiter mass|link=yes}}33010 AU318Candidate Jupiter-mass satellite from direct imaging. If confirmed, it could also be considered a planet orbiting a brown dwarf.{{cite journal |last=Lazzoni |first=C. |display-authors=etal |date=20 July 2020 |title=The search for disks or planetary objects around directly imaged companions: A candidate around DH Tau B |journal=Astronomy & Astrophysics |volume=641 |pages=A131 |doi=10.1051/0004-6361/201937290 |arxiv=2007.10097|bibcode=2020A&A...641A.131L |s2cid=220647289 }}
rowspan="2" | HD 189733rowspan="2" | HD 189733 browspan="2" | 1.13 {{Jupiter mass|link=yes}}rowspan="2" | 0.0310.0087 AU?Found by studying periodic increases and decreases in light given off from HD 189733 b. Outside of planet's Hill sphere.{{cite journal |last1=Ben-Jaffel |first1=Lotfi |last2=Ballester |first2=Gilda |arxiv=1404.1084 |title=Transit of Exomoon Plasma Tori: New Diagnosis |journal=The Astrophysical Journal |date=3 April 2014 |volume=785 |issue=2 |pages=L30 |doi=10.1088/2041-8205/785/2/L30 |bibcode=2014ApJ...785L..30B |s2cid=119282630 }}
<0.00112 AU~ 0.015Exo-Io candidate; The sodium and potassium data{{cite journal |last1=Wyttenbach |first1=A. |last2=Ehrenreich |first2=D. |last3=Lovis |first3=C. |last4=Udry |first4=S. |last5=Pepe |first5=F. |title=Spectrally resolved detection of sodium in the atmosphere of HD 189733b with the HARPS spectrograph |journal=Astronomy & Astrophysics |date=5 May 2015 |volume=577 |page=A62 |doi=10.1051/0004-6361/201525729 |arxiv=1503.05581 |bibcode=2015A&A...577A..62W |s2cid=54935174 |url=https://www.aanda.org/articles/aa/full_html/2015/05/aa25729-15/aa25729-15.html}}{{cite journal |last1=Keles |first1=Engin |last2=Mallonn |first2=Matthias |last3=von Essen |first3=Carolina |last4=Carroll |first4=Thorsten |last5=Alexoudi |first5=Xanthippi |last6=Pino |first6=Lorenzo |last7=Ilyin |first7=Ilya |last8=Poppenhager |first8=Katja |last9=Kitzmann |first9=Daniel |last10=Nascimbeni |first10=Valerio |last11=Turner |first11=Jake D |last12=Strassmeier |first12=Klaus G |title=The potassium absorption on HD189733b and HD209458b |journal=Monthly Notices of the Royal Astronomical Society: Letters |date=October 2019 |volume=489 |issue=1 |page=L37-L41 |doi=10.1093/mnrasl/slz123|doi-access=free |arxiv=1909.04884 |bibcode=2019MNRAS.489L..37K |s2cid=202134796 }} at HD 189733b is consistent with evaporating exomoons and/or their corresponding gas torus.{{cite journal |last1=Gebek |first1=Andrea |last2=Oza |first2=Apurva |title=Alkaline exospheres of exoplanet systems: evaporative transmission spectra |journal=Monthly Notices of the Royal Astronomical Society |date=29 July 2020 |volume=497 |issue=4 |pages=5271–5291 |doi=10.1093/mnras/staa2193 |doi-access=free |arxiv=2005.02536 |bibcode=2020MNRAS.497.5271G |s2cid=218516741 |url=https://academic.oup.com/mnras/article-abstract/497/4/5271/5877918?redirectedFrom=fulltext |access-date=8 December 2020}}
Kepler-409Kepler-409b1.00 {{Earth mass|sym=y|link=yes}}0.3200.222 RHill0.300Possible exomoon from transit timing variations, since deemed unlikely.
Kepler-517Kepler-517b7.59 {{Earth mass|sym=y|link=yes}}0.2980.278 RHill0.499Possible exomoon from transit timing variations, since deemed unlikely.
Kepler-809Kepler-809b38.02 {{Earth mass|sym=y|link=yes}}0.3080.289 RHill2.931Possible exomoon from transit timing variations.
Kepler-857Kepler-857b14.13 {{Earth mass|sym=y|link=yes}}0.3760.208 RHill1.636Possible exomoon from transit timing variations.
Kepler-1000Kepler-1000b19.95 {{Earth mass|sym=y|link=yes}}0.5340.235 RHill1.551Possible exomoon from transit timing variations, since deemed unlikely.
Kepler-1326Kepler-1326b24.55 {{Earth mass|sym=y|link=yes}}0.26910.295 RHill6.057Possible exomoon from transit timing variations, since deemed unlikely.
Kepler-1442Kepler-1442b14.13 {{Earth mass|sym=y|link=yes}}0.4050.208 RHill1.586Possible exomoon from transit timing variations, since deemed unlikely.
Kepler-1625Kepler-1625b{{sort|11.6|<11.6}} {{Jupiter mass|link=yes}}{{cite journal |last1=Timmermann |first1=Anina |display-authors=etal |arxiv=2001.10867 |title=Radial velocity constraints on the long-period transiting planet Kepler-1625 b with CARMENES |journal=Astronomy & Astrophysics |date=29 January 2020 |volume=635 |pages=A59 |doi=10.1051/0004-6361/201937325 |bibcode=2020A&A...635A..59T |s2cid=210942758 }}0.980.022 AU19.0Possible Neptune-sized exomoon or double planet, indicated by transit observations.{{cite news |last=Drake |first=Nadia |author-link=Nadia Drake |title=Weird giant may be the first known alien moon – Evidence is mounting that a world the size of Neptune could be orbiting a giant planet far, far away. |url=https://www.nationalgeographic.com/science/2018/10/news-first-exomoon-nasa-kepler-planets-facts-space/ |archive-url=https://web.archive.org/web/20181003234439/https://www.nationalgeographic.com/science/2018/10/news-first-exomoon-nasa-kepler-planets-facts-space/ |url-status=dead |archive-date=3 October 2018 |date=3 October 2018 |work=National Geographic Society |access-date=4 October 2018 }}
Kepler-1708Kepler-1708b{{sort|4.6|<4.6}} {{Jupiter mass|link=yes}}1.640.005 AU
(11.7 RP)		{{sort|37|<37}}Possible Neptune-sized exomoon or double planet, indicated by transit observations.
KOI-268KOI-268.019.33 {{Earth mass|sym=y|link=yes}}0.470.217 RHill0.817Possible exomoon from transit timing variations, since deemed unlikely.
N/AMOA-2015-BLG-337L9.85 {{Jupiter mass|link=yes}}N/A0.24 AU33.7Found by microlensing; however it is unknown if the system is a super-Neptune-mass planet orbiting a free-floating planet, or a binary brown dwarf system.{{cite journal |last1=Miyazaki |first1=S. |display-authors=etal |arxiv=1804.00830 |title=MOA-2015-BLG-337: A Planetary System with a Low-mass Brown Dwarf/Planetary Boundary Host, or a Brown Dwarf Binary |journal=The Astronomical Journal |date=24 July 2018 |volume=156 |issue=3 |pages=136 |doi=10.3847/1538-3881/aad5ee |bibcode=2018AJ....156..136M |s2cid=58928147 |doi-access=free }}
rowspan="2" |WASP-12

| rowspan="2" |WASP-12b{{cite encyclopedia|title=WASP-12 b|url=https://exoplanet.eu/catalog/wasp_12_b--459/|access-date=1 February 2015|url-status=live|archive-url=https://web.archive.org/web/20150201211333/http://exoplanet.eu/catalog/wasp-12_b/|encyclopedia=Extrasolar Planets Encyclopaedia|archive-date=1 February 2015}}

| rowspan="2" |1.465 {{Jupiter mass|link=yes}}

| rowspan="2" |0.0232

|

|{{sort|03.485|6.4}} (radius)[http://www.ria.ru/science/20120206/558647431.html Российские астрономы впервые открыли луну возле экзопланеты] (in Russian) - "Studying of a curve of change of shine of WASP-12b has brought to the Russian astronomers unusual result: regular splashes were found out.<...> Though stains on a star surface also can cause similar changes of shine, observable splashes are very similar on duration, a profile and amplitude that testifies for benefit of exomoon existence."

|

6 RPFound by studying periodic increases and decreases in light given off from WASP-12b. Outside of planet's Hill sphere.
WASP-49WASP-49b0.37 {{Jupiter mass|link=yes}}0.0379< 1.74 RP~ 0.015Exo-Io candidate; The sodium exosphere around WASP-49b could be due to a volcanically active Io-like exomoon.{{Cite journal|last1=Oza|first1=Apurva V.|last2=Johnson|first2=Robert E.|last3=Lellouch|first3=Emmanuel|last4=Schmidt|first4=Carl|last5=Schneider|first5=Nick|last6=Huang|first6=Chenliang|last7=Gamborino|first7=Diana|last8=Gebek|first8=Andrea|last9=Wyttenbach|first9=Aurelien|last10=Demory|first10=Brice-Olivier|last11=Mordasini|first11=Christoph|first12=Prabal|last12=Saxena|first13=David |last13=Dubois|first14=Arielle |last14=Moullet|first15=Nicolas |last15=Thomas|date=2019-08-28|title=Sodium and Potassium Signatures of Volcanic Satellites Orbiting Close-in Gas Giant Exoplanets|arxiv=1908.10732 |bibcode=2019ApJ...885..168O |doi=10.3847/1538-4357/ab40cc |journal=The Astrophysical Journal|volume=885|issue=2|pages=168|s2cid=201651224 |doi-access=free }}
WASP-76WASP-76b0.92 {{Jupiter mass|link=yes}}0.0331.125 RP~ 0.015Exo-Io candidate; Sodium detected via absorption spectroscopy around WASP-76b{{cite journal |last1=Seidel |first1=J.V. |last2=Ehrenreich |first2=D. |last3=Wyttenbach |first3=A. |last4=Allart |first4=R. |last5=Lendl |first5=M. |last6=Pino |first6=L. |last7=Bourrier |first7=V. |last8=Cegla |first8=H.M. |last9=Lovis |first9=C. |last10=Barrado |first10=D. |last11=Bayliss |first11=D. |last12=Astudillo-Defru |first12=N. |last13=Deline |first13=A. |last14=Fisher |first14=C. |last15=Heng |first15=K. |last16=Joseph |first16=R. |last17=Lavie |first17=B. |last18=Melo |first18=C. |last19=Pepe |first19=F. |last20=Segransan |first20=D. |last21=Udry |first21=S. |title=Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS)★ II. A broadened sodium feature on the ultra-hot giant WASP-76b |journal=Astronomy & Astrophysics |date=27 March 2019 |volume=623 |page=A166 |doi=10.1051/0004-6361/201834776|arxiv=1902.00001 |bibcode=2019A&A...623A.166S |s2cid=119348582 }} is consistent with an extrasolar toroidal atmosphere{{cite journal |last1=Johnson |first1=Robert E. |last2=Huggins |first2=Patrick |title=Toroidal Atmospheres around Extrasolar Planets |journal=Publications of the Astronomical Society of the Pacific |date=August 2006 |volume=118 |issue=846 |pages=1136–1143 |doi=10.1086/506183|arxiv=astro-ph/0605655 |bibcode=2006PASP..118.1136J |s2cid=16201558 }} generated by an evaporating exomoon.
WASP-121WASP-121b1.184 {{Jupiter mass|link=yes}}0.02544~ 1.9 RP~ 0.015Exo-Io candidate; The sodium detected via absorption spectroscopy around WASP-121b{{cite journal |last1=Hoeijmakers |first1=H.J. |last2=Seidel |first2=J.V. |last3=Pino |first3=L. |last4=Kitzmann |first4=D. |last5=Sindel |first5=J.P. |last6=Ehrenreich |first6=D. |last7=Oza |first7=A.V. |last8=Bourrier |first8=V. |last9=Allart |first9=R. |last10=Gebek |first10=A. |last11=Lovis |first11=C. |last12=Yurchenko |first12=S.N. |last13=Astudillo-Defru |first13=N. |last14=Bayliss |first14=D. |last15=Cegla |first15=H. |last16=Lavie |first16=B. |last17=Lendl |first17=M. |last18=Melo |first18=C. |last19=Murgas |first19=F. |last20=Nascimbeni |first20=V. |last21=Pepe |first21=F. |last22=Segransan |first22=D. |last23=Udry |first23=S. |last24=Wyttenbach |first24=A. |last25=Heng |first25=K. |title=Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS) - IV. A spectral inventory of atoms and molecules in the high-resolution transmission spectrum of WASP-121 b |journal=Astronomy & Astrophysics |date=18 September 2020 |volume=641 |page=A123 |doi=10.1051/0004-6361/202038365|arxiv=2006.11308 |bibcode=2020A&A...641A.123H |s2cid=219966241 }} is consistent with an extrasolar gas torus possibly fueled by a hidden exo-Io.

References

{{Reflist|refs=

{{cite journal|author=Matthew A. Kenworthy, Eric E. Mamajek|title=Modeling giant extrasolar ring systems in eclipse and the case of J1407b: sculpting by exomoons?|journal=The Astrophysical Journal|volume=800|issue=2|pages=126|arxiv=1501.05652 |year=2015|bibcode = 2015ApJ...800..126K |doi = 10.1088/0004-637X/800/2/126 |s2cid=56118870}}

{{cite journal |last1=Kenworthy |first1=M. A. |last2=Klaassen |first2=P. D. |display-authors=etal |date=January 2020 |title=ALMA and NACO observations towards the young exoring transit system J1407 (V1400 Cen) |journal=Astronomy & Astrophysics |volume=633 |issue= |pages=A115 |doi=10.1051/0004-6361/201936141 |arxiv=1912.03314 |bibcode=2020A&A...633A.115K}}

{{Cite journal |last1=Terry |first1=Sean K. |title=A Candidate High-velocity Exoplanet System in the Galactic Bulge |date=2025 |arxiv=2410.09147 |last2=Beaulieu |first2=Jean-Philippe |last3=Bennett |first3=David P. |last4=Bhattacharya |first4=Aparna |last5=Hulberg |first5=Jon |last6=Huston |first6=Macy J. |last7=Koshimoto |first7=Naoki |last8=Blackman |first8=Joshua W. |last9=Bond |first9=Ian A.|journal=The Astronomical Journal |volume=169 |issue=3 |page=131 |doi=10.3847/1538-3881/ad9b0f |doi-access=free |bibcode=2025AJ....169..131T }}

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{{DEFAULTSORT:Exomoon candidates}}

Exomoon candidates

Category:Exomoons