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List of exoplanets detected by microlensing: Difference between revisions

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This is a '''list of ]s detected by ]'''. The phenomenon results in the background star's light being warped around a foreground object, causing a distorted image. If the foreground object is a star with an orbiting ], we would observe an abnormally ] image. By comparing the luminosity and light distortion of the background star to theoretical models, we can estimate the planet's mass and the distance from its star. This is a '''list of ]s detected by ]'''. The phenomenon results in the background star's light being warped around a foreground object, causing a distorted image. If the foreground object is a star with an orbiting ], we would observe an abnormally ] image. By comparing the luminosity and light distortion of the background star to theoretical models, we can estimate the planet's mass and the distance from its star.


The least massive planet detected by microlensing is KMT-2020-BLG-0414Lb, which has about the same mass as ]. The widest separation between a planet and a star is OGLE-2008-BLG-092Lb, which is ~18 ]; the shortest separation is KMT-2020-BLG-0414Lc, which is 0.12 AU. There are 7 known ] detected by microlensing, all of which have two planets.<ref>{{cite web |title=Planetary Systems Composite Data |url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=PSCompPars |website=] |accessdate=19 February 2023}}</ref> The least massive planet detected by microlensing is ]<nowiki/>b, which has a mass about 1.9 times the mass of ], or OGLE-2013-BLG-0341LBb, which has a mass about 2 times the mass of earth.<ref name="Zhang2024">{{cite journal |last1=Zhang |first1=Keming |last2=Zang |first2=Weicheng |last3=El-Badry |first3=Kareem |last4=Lu |first4=Jessica R. |display-authors=etal |date=September 2024 |title=An Earth-Mass Planet and a Brown Dwarf in Orbit Around a White Dwarf |journal=Accepted for publication |volume= |issue= |pages= |arxiv=2409.02157 |doi=}}</ref><ref name="Gould_2014" /> The widest separation between a planet and a star is OGLE-2008-BLG-092Lb, which is ~18 ]; the shortest separation is MOA-2015-BLG-337Lb, which is 0.24 AU. There are 7 known ] detected by microlensing, all of which have two planets.<ref>{{cite web |title=Planetary Systems Composite Data |url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=PSCompPars |website=] |accessdate=19 February 2023}}</ref>


== List == == List ==
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| OGLE-2012-BLG-0950Lb || 0.079 || 2.2 || || || || 2016<ref name="Koshimoto2016"/> | OGLE-2012-BLG-0950Lb || 0.079 || 2.2 || || || || 2016<ref name="Koshimoto2016"/>
|- bgcolor="#7fffb0" |- bgcolor="#7fffb0"
| ] || 0.25 || 2.59 || 2557 || || || 2016<ref name="Bennett2016"/> | ] || 0.25 || 2.59 || 2557 || || || 2016<ref name="Bennett2016"/>
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| OGLE-2014-BLG-0676Lb || 3.68 || 4.53 || || || || 2016<ref name="Rattenbury2017"/> | OGLE-2014-BLG-0676Lb || 3.68 || 4.53 || || || || 2016<ref name="Rattenbury2017"/>
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|2018<ref>{{Cite journal |last1=Nucita |first1=A. A. |last2=Licchelli |first2=D. |last3=De Paolis |first3=F. |last4=Ingrosso |first4=G. |last5=Strafella |first5=F. |last6=Katysheva |first6=N. |last7=Shugarov |first7=S. |date=2018-05-01 |title=Discovery of a bright microlensing event with planetary features towards the Taurus region: a super-Earth planet |url=https://ui.adsabs.harvard.edu/abs/2018MNRAS.476.2962N |journal=Monthly Notices of the Royal Astronomical Society |volume=476 |issue=3 |pages=2962–2967 |doi=10.1093/mnras/sty448 |arxiv=1802.06659 |bibcode=2018MNRAS.476.2962N |issn=0035-8711}}</ref><ref>{{Cite journal |last1=Zang |first1=Weicheng |last2=Dong |first2=Subo |last3=Gould |first3=Andrew |last4=Calchi Novati |first4=Sebastiano |last5=Chen |first5=Ping |last6=Yang |first6=Hongjing |last7=Li |first7=Shun-Sheng |last8=Mao |first8=Shude |last9=Alton |first9=K. B. |last10=Brimacombe |first10=J. |last11=Carey |first11=Sean |last12=Christie |first12=G. W. |last13=Delplancke-Ströbele |first13=F. |last14=Feliz |first14=Dax L. |last15=Gaudi |first15=B. Scott |date=2020-07-01 |title=Spitzer + VLTI-GRAVITY Measure the Lens Mass of a Nearby Microlensing Event |journal=The Astrophysical Journal |volume=897 |issue=2 |pages=180 |doi=10.3847/1538-4357/ab9749 |doi-access=free |arxiv=1912.00038 |bibcode=2020ApJ...897..180Z |issn=0004-637X}}</ref><ref>{{Cite journal |last1=Fukui |first1=A. |last2=Suzuki |first2=D. |last3=Koshimoto |first3=N. |last4=Bachelet |first4=E. |last5=Vanmunster |first5=T. |last6=Storey |first6=D. |last7=Maehara |first7=H. |last8=Yanagisawa |first8=K. |last9=Yamada |first9=T. |last10=Yonehara |first10=A. |last11=Hirano |first11=T. |last12=Bennett |first12=D. P. |last13=Bozza |first13=V. |last14=Mawet |first14=D. |last15=Penny |first15=M. T. |date=2019-11-01 |title=Kojima-1Lb Is a Mildly Cold Neptune around the Brightest Microlensing Host Star |journal=The Astronomical Journal |volume=158 |issue=5 |pages=206 |doi=10.3847/1538-3881/ab487f |doi-access=free |arxiv=1909.11802 |bibcode=2019AJ....158..206F |issn=0004-6256}}</ref> |2018<ref>{{Cite journal |last1=Nucita |first1=A. A. |last2=Licchelli |first2=D. |last3=De Paolis |first3=F. |last4=Ingrosso |first4=G. |last5=Strafella |first5=F. |last6=Katysheva |first6=N. |last7=Shugarov |first7=S. |date=2018-05-01 |title=Discovery of a bright microlensing event with planetary features towards the Taurus region: a super-Earth planet |journal=Monthly Notices of the Royal Astronomical Society |volume=476 |issue=3 |pages=2962–2967 |doi=10.1093/mnras/sty448 |doi-access=free |arxiv=1802.06659 |bibcode=2018MNRAS.476.2962N |issn=0035-8711}}</ref><ref>{{Cite journal |last1=Zang |first1=Weicheng |last2=Dong |first2=Subo |last3=Gould |first3=Andrew |last4=Calchi Novati |first4=Sebastiano |last5=Chen |first5=Ping |last6=Yang |first6=Hongjing |last7=Li |first7=Shun-Sheng |last8=Mao |first8=Shude |last9=Alton |first9=K. B. |last10=Brimacombe |first10=J. |last11=Carey |first11=Sean |last12=Christie |first12=G. W. |last13=Delplancke-Ströbele |first13=F. |last14=Feliz |first14=Dax L. |last15=Gaudi |first15=B. Scott |date=2020-07-01 |title=Spitzer + VLTI-GRAVITY Measure the Lens Mass of a Nearby Microlensing Event |journal=The Astrophysical Journal |volume=897 |issue=2 |pages=180 |doi=10.3847/1538-4357/ab9749 |doi-access=free |arxiv=1912.00038 |bibcode=2020ApJ...897..180Z |issn=0004-637X}}</ref><ref>{{Cite journal |last1=Fukui |first1=A. |last2=Suzuki |first2=D. |last3=Koshimoto |first3=N. |last4=Bachelet |first4=E. |last5=Vanmunster |first5=T. |last6=Storey |first6=D. |last7=Maehara |first7=H. |last8=Yanagisawa |first8=K. |last9=Yamada |first9=T. |last10=Yonehara |first10=A. |last11=Hirano |first11=T. |last12=Bennett |first12=D. P. |last13=Bozza |first13=V. |last14=Mawet |first14=D. |last15=Penny |first15=M. T. |date=2019-11-01 |title=Kojima-1Lb Is a Mildly Cold Neptune around the Brightest Microlensing Host Star |journal=The Astronomical Journal |volume=158 |issue=5 |pages=206 |doi=10.3847/1538-3881/ab487f |doi-access=free |arxiv=1909.11802 |bibcode=2019AJ....158..206F |issn=0004-6256}}</ref>
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|2021<ref>{{Cite journal |last1=Kim |first1=Yun Hak |last2=Chung |first2=Sun-Ju |last3=Udalski |first3=Andrej |last4=Gould |first4=Andrew |last5=Albrow |first5=Michael D. |last6=Jung |first6=Youn Kil |last7=Hwang |first7=Kyu-Ha |last8=Han |first8=Cheongho |last9=Ryu |first9=Yoon-Hyun |last10=Shin |first10=In-Gu |last11=Shvartzvald |first11=Yossi |last12=Yee |first12=Jennifer C. |last13=Zang |first13=Weicheng |last14=Cha |first14=Sang-Mok |last15=Kim |first15=Dong-Jin |date=2021-05-01 |title=OGLE-2018-BLG-1428Lb: a Jupiter-mass planet beyond the snow line of a dwarf star |url=https://ui.adsabs.harvard.edu/abs/2021MNRAS.503.2706K |journal=Monthly Notices of the Royal Astronomical Society |volume=503 |issue=2 |pages=2706–2712 |doi=10.1093/mnras/stab534 |arxiv=2102.11463 |bibcode=2021MNRAS.503.2706K |issn=0035-8711}}</ref> |2021<ref>{{Cite journal |last1=Kim |first1=Yun Hak |last2=Chung |first2=Sun-Ju |last3=Udalski |first3=Andrej |last4=Gould |first4=Andrew |last5=Albrow |first5=Michael D. |last6=Jung |first6=Youn Kil |last7=Hwang |first7=Kyu-Ha |last8=Han |first8=Cheongho |last9=Ryu |first9=Yoon-Hyun |last10=Shin |first10=In-Gu |last11=Shvartzvald |first11=Yossi |last12=Yee |first12=Jennifer C. |last13=Zang |first13=Weicheng |last14=Cha |first14=Sang-Mok |last15=Kim |first15=Dong-Jin |date=2021-05-01 |title=OGLE-2018-BLG-1428Lb: a Jupiter-mass planet beyond the snow line of a dwarf star |journal=Monthly Notices of the Royal Astronomical Society |volume=503 |issue=2 |pages=2706–2712 |doi=10.1093/mnras/stab534 |doi-access=free |arxiv=2102.11463 |bibcode=2021MNRAS.503.2706K |issn=0035-8711}}</ref>
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|OGLE-2018-BLG-1185Lb |OGLE-2018-BLG-1185Lb
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|2021<ref>{{Cite journal |last1=Han |first1=Cheongho |last2=Gould |first2=Andrew |last3=Hirao |first3=Yuki |last4=Lee |first4=Chung-Uk |last5=Albrow |first5=Michael D. |last6=Chung |first6=Sun-Ju |last7=Hwang |first7=Kyu-Ha |last8=Jung |first8=Youn Kil |last9=Kim |first9=Doeon |last10=Mao |first10=Shude |last11=Ryu |first11=Yoon-Hyun |last12=Shin |first12=In-Gu |last13=Shvartzvald |first13=Yossi |last14=Yee |first14=Jennifer C. |last15=Zang |first15=Weicheng |date=2021-11-01 |title=KMT-2021-BLG-0322: Severe degeneracy between triple-lens and higher-order binary-lens interpretations |url=https://ui.adsabs.harvard.edu/abs/2021A&A...655A..24H |journal=Astronomy and Astrophysics |volume=655 |pages=A24 |doi=10.1051/0004-6361/202141939 |arxiv=2109.02210 |bibcode=2021A&A...655A..24H |issn=0004-6361}}</ref> |2021<ref>{{Cite journal |last1=Han |first1=Cheongho |last2=Gould |first2=Andrew |last3=Hirao |first3=Yuki |last4=Lee |first4=Chung-Uk |last5=Albrow |first5=Michael D. |last6=Chung |first6=Sun-Ju |last7=Hwang |first7=Kyu-Ha |last8=Jung |first8=Youn Kil |last9=Kim |first9=Doeon |last10=Mao |first10=Shude |last11=Ryu |first11=Yoon-Hyun |last12=Shin |first12=In-Gu |last13=Shvartzvald |first13=Yossi |last14=Yee |first14=Jennifer C. |last15=Zang |first15=Weicheng |date=2021-11-01 |title=KMT-2021-BLG-0322: Severe degeneracy between triple-lens and higher-order binary-lens interpretations |url=https://ui.adsabs.harvard.edu/abs/2021A&A...655A..24H |journal=Astronomy and Astrophysics |volume=655 |pages=A24 |doi=10.1051/0004-6361/202141939 |arxiv=2109.02210 |bibcode=2021A&A...655A..24H |issn=0004-6361}}</ref>
|- bgcolor="#ffffb0" |- bgcolor="#ffffb0"
|KMT-2020-BLG-0414Lb |]<nowiki/>b
|0.00381 |0.00588
|1.79 |2.07
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|2021<ref name=":4">{{Cite journal |last1=Zang |first1=Weicheng |last2=Han |first2=Cheongho |last3=Kondo |first3=Iona |last4=Yee |first4=Jennifer C. |last5=Lee |first5=Chung-Uk |last6=Gould |first6=Andrew |last7=Mao |first7=Shude |last8=de Almeida |first8=Leandro |last9=Shvartzvald |first9=Yossi |last10=Zhang |first10=Xiangyu |last11=Albrow |first11=Michael D. |last12=Chung |first12=Sun-Ju |last13=Hwang |first13=Kyu-Ha |last14=Jung |first14=Youn Kil |last15=Ryu |first15=Yoon-Hyun |date=2021-11-01 |title=An Earth-mass planet in a time of COVID-19: KMT-2020-BLG-0414Lb |url=https://iopscience.iop.org/article/10.1088/1674-4527/21/9/239 |journal=Research in Astronomy and Astrophysics |volume=21 |issue=9 |pages=239 |doi=10.1088/1674-4527/21/9/239 |arxiv=2103.01896 |bibcode=2021RAA....21..239Z |issn=1674-4527}}</ref> |2021<ref name=":4">{{Cite journal |last1=Zang |first1=Weicheng |last2=Han |first2=Cheongho |last3=Kondo |first3=Iona |last4=Yee |first4=Jennifer C. |last5=Lee |first5=Chung-Uk |last6=Gould |first6=Andrew |last7=Mao |first7=Shude |last8=de Almeida |first8=Leandro |last9=Shvartzvald |first9=Yossi |last10=Zhang |first10=Xiangyu |last11=Albrow |first11=Michael D. |last12=Chung |first12=Sun-Ju |last13=Hwang |first13=Kyu-Ha |last14=Jung |first14=Youn Kil |last15=Ryu |first15=Yoon-Hyun |date=2021-11-01 |title=An Earth-mass planet in a time of COVID-19: KMT-2020-BLG-0414Lb |url=https://iopscience.iop.org/article/10.1088/1674-4527/21/9/239 |journal=Research in Astronomy and Astrophysics |volume=21 |issue=9 |pages=239 |doi=10.1088/1674-4527/21/9/239 |arxiv=2103.01896 |bibcode=2021RAA....21..239Z |issn=1674-4527}}</ref><ref name="Zhang2024" />
|- bgcolor="#ffffb0" |- bgcolor="#ffffb0"
|KMT-2020-BLG-0414Lc |]<nowiki/>c
|27
|15.4
|0.12 |22.3
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|2021<ref name=":4" /> |2021<ref name=":4" /><ref name="Zhang2024" />
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|KMT-2019-BLG-1715Lb |KMT-2019-BLG-1715Lb
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|2022<ref>{{Cite journal |last1=Kuang |first1=Renkun |last2=Zang |first2=Weicheng |last3=Jung |first3=Youn Kil |last4=Udalski |first4=Andrzej |last5=Yang |first5=Hongjing |last6=Mao |first6=Shude |last7=Albrow |first7=Michael D. |last8=Chung |first8=Sun-Ju |last9=Gould |first9=Andrew |last10=Han |first10=Cheongho |last11=Hwang |first11=Kyu-Ha |last12=Ryu |first12=Yoon-Hyun |last13=Shin |first13=In-Gu |last14=Shvartzvald |first14=Yossi |last15=Yee |first15=Jennifer C. |date=2022-10-01 |title=OGLE-2019-BLG-1470LABc: Another microlensing giant planet in a binary system? |url=https://ui.adsabs.harvard.edu/abs/2022MNRAS.516.1704K |journal=Monthly Notices of the Royal Astronomical Society |volume=516 |issue=2 |pages=1704–1720 |doi=10.1093/mnras/stac2315 |arxiv=2204.05606 |bibcode=2022MNRAS.516.1704K |issn=0035-8711}}</ref> |2022<ref>{{Cite journal |last1=Kuang |first1=Renkun |last2=Zang |first2=Weicheng |last3=Jung |first3=Youn Kil |last4=Udalski |first4=Andrzej |last5=Yang |first5=Hongjing |last6=Mao |first6=Shude |last7=Albrow |first7=Michael D. |last8=Chung |first8=Sun-Ju |last9=Gould |first9=Andrew |last10=Han |first10=Cheongho |last11=Hwang |first11=Kyu-Ha |last12=Ryu |first12=Yoon-Hyun |last13=Shin |first13=In-Gu |last14=Shvartzvald |first14=Yossi |last15=Yee |first15=Jennifer C. |date=2022-10-01 |title=OGLE-2019-BLG-1470LABc: Another microlensing giant planet in a binary system? |journal=Monthly Notices of the Royal Astronomical Society |volume=516 |issue=2 |pages=1704–1720 |doi=10.1093/mnras/stac2315 |doi-access=free |arxiv=2204.05606 |bibcode=2022MNRAS.516.1704K |issn=0035-8711}}</ref>
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|OGLE-2019-BLG-1492Lb |OGLE-2019-BLG-1492Lb
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|2022<ref>{{Cite journal |last1=Chung |first1=Sun-Ju |last2=Yee |first2=Jennifer C. |last3=Udalski |first3=Andrej |last4=Gould |first4=Andrew |last5=Albrow |first5=Michael D. |last6=Jung |first6=Youn Kil |last7=Hwang |first7=Kyu-Ha |last8=Han |first8=Cheongho |last9=Ryu |first9=Yoon-Hyun |last10=Shin |first10=In-Gu |last11=Shvartzvald |first11=Yossi |last12=Zang |first12=Weicheng |last13=Cha |first13=Sang-Mok |last14=Kim |first14=Dong-Jin |last15=Kim |first15=Seung-Lee |date=2022-08-01 |title=OGLE-2019-BLG-0362Lb: A Super-Jovian-Mass Planet around a Low-Mass Star |url=https://ui.adsabs.harvard.edu/abs/2022JKAS...55..123C |journal=Journal of Korean Astronomical Society |volume=55 |pages=123–130 |doi=10.5303/JKAS.2022.55.4.123 |arxiv=2208.04230 |bibcode=2022JKAS...55..123C |issn=1225-4614}}</ref> |2022<ref>{{Cite journal |last1=Chung |first1=Sun-Ju |last2=Yee |first2=Jennifer C. |last3=Udalski |first3=Andrej |last4=Gould |first4=Andrew |last5=Albrow |first5=Michael D. |last6=Jung |first6=Youn Kil |last7=Hwang |first7=Kyu-Ha |last8=Han |first8=Cheongho |last9=Ryu |first9=Yoon-Hyun |last10=Shin |first10=In-Gu |last11=Shvartzvald |first11=Yossi |last12=Zang |first12=Weicheng |last13=Cha |first13=Sang-Mok |last14=Kim |first14=Dong-Jin |last15=Kim |first15=Seung-Lee |date=2022-08-01 |title=OGLE-2019-BLG-0362Lb: A Super-Jovian-Mass Planet around a Low-Mass Star |url=https://ui.adsabs.harvard.edu/abs/2022JKAS...55..123C |journal=Journal of Korean Astronomical Society |volume=55 |issue=4 |pages=123–130 |doi=10.5303/JKAS.2022.55.4.123 |arxiv=2208.04230 |bibcode=2022JKAS...55..123C |issn=1225-4614}}</ref>
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|OGLE-2018-BLG-1647Lb |OGLE-2018-BLG-1647Lb
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|2022<ref>{{Cite journal |last1=Wang |first1=Hanyue |last2=Zang |first2=Weicheng |last3=Zhu |first3=Wei |last4=Hwang |first4=Kyu-Ha |last5=Udalski |first5=Andrzej |last6=Gould |first6=Andrew |last7=Han |first7=Cheongho |last8=Albrow |first8=Michael D. |last9=Chung |first9=Sun-Ju |last10=Jung |first10=Youn Kil |last11=Kim |first11=Doeon |last12=Ryu |first12=Yoon-Hyun |last13=Shin |first13=In-Gu |last14=Shvartzvald |first14=Yossi |last15=Yee |first15=Jennifer C. |date=2022-02-01 |title=Systematic Korea Microlensing Telescope Network planetary anomaly search - III. One wide-orbit planet and two stellar binaries |url=https://ui.adsabs.harvard.edu/abs/2022MNRAS.510.1778W |journal=Monthly Notices of the Royal Astronomical Society |volume=510 |issue=2 |pages=1778–1790 |doi=10.1093/mnras/stab3581 |arxiv=2112.02414 |bibcode=2022MNRAS.510.1778W |issn=0035-8711}}</ref> |2022<ref>{{Cite journal |last1=Wang |first1=Hanyue |last2=Zang |first2=Weicheng |last3=Zhu |first3=Wei |last4=Hwang |first4=Kyu-Ha |last5=Udalski |first5=Andrzej |last6=Gould |first6=Andrew |last7=Han |first7=Cheongho |last8=Albrow |first8=Michael D. |last9=Chung |first9=Sun-Ju |last10=Jung |first10=Youn Kil |last11=Kim |first11=Doeon |last12=Ryu |first12=Yoon-Hyun |last13=Shin |first13=In-Gu |last14=Shvartzvald |first14=Yossi |last15=Yee |first15=Jennifer C. |date=2022-02-01 |title=Systematic Korea Microlensing Telescope Network planetary anomaly search - III. One wide-orbit planet and two stellar binaries |journal=Monthly Notices of the Royal Astronomical Society |volume=510 |issue=2 |pages=1778–1790 |doi=10.1093/mnras/stab3581 |doi-access=free |arxiv=2112.02414 |bibcode=2022MNRAS.510.1778W |issn=0035-8711}}</ref>
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|OGLE-2017-BLG-1691Lb |OGLE-2017-BLG-1691Lb
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|2022<ref>{{Cite journal |last1=Zang |first1=Weicheng |last2=Shvartzvald |first2=Yossi |last3=Udalski |first3=Andrzej |last4=Yee |first4=Jennifer C. |last5=Lee |first5=Chung-Uk |last6=Sumi |first6=Takahiro |last7=Zhang |first7=Xiangyu |last8=Yang |first8=Hongjing |last9=Mao |first9=Shude |last10=Novati |first10=Sebastiano Calchi |last11=Gould |first11=Andrew |last12=Zhu |first12=Wei |last13=Beichman |first13=Charles A. |last14=Bryden |first14=Geoffery |last15=Carey |first15=Sean |date=2022-08-01 |title=OGLE-2018-BLG-0799Lb: a q 2.7 × 10-3 planet with Spitzer parallax |url=https://ui.adsabs.harvard.edu/abs/2022MNRAS.514.5952Z |journal=Monthly Notices of the Royal Astronomical Society |volume=514 |issue=4 |pages=5952–5968 |doi=10.1093/mnras/stac1631 |arxiv=2010.08732 |bibcode=2022MNRAS.514.5952Z |issn=0035-8711}}</ref> |2022<ref>{{Cite journal |last1=Zang |first1=Weicheng |last2=Shvartzvald |first2=Yossi |last3=Udalski |first3=Andrzej |last4=Yee |first4=Jennifer C. |last5=Lee |first5=Chung-Uk |last6=Sumi |first6=Takahiro |last7=Zhang |first7=Xiangyu |last8=Yang |first8=Hongjing |last9=Mao |first9=Shude |last10=Novati |first10=Sebastiano Calchi |last11=Gould |first11=Andrew |last12=Zhu |first12=Wei |last13=Beichman |first13=Charles A. |last14=Bryden |first14=Geoffery |last15=Carey |first15=Sean |date=2022-08-01 |title=OGLE-2018-BLG-0799Lb: a q 2.7 × 10-3 planet with Spitzer parallax |journal=Monthly Notices of the Royal Astronomical Society |volume=514 |issue=4 |pages=5952–5968 |doi=10.1093/mnras/stac1631 |doi-access=free |arxiv=2010.08732 |bibcode=2022MNRAS.514.5952Z |issn=0035-8711}}</ref>
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|OGLE-2018-BLG-0932Lb |OGLE-2018-BLG-0932Lb
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|2022<ref name=":16">{{Cite journal |last1=Yang |first1=Hongjing |last2=Zang |first2=Weicheng |last3=Gould |first3=Andrew |last4=Yee |first4=Jennifer C. |last5=Hwang |first5=Kyu-Ha |last6=Christie |first6=Grant |last7=Sumi |first7=Takahiro |last8=Zhang |first8=Jiyuan |last9=Mao |first9=Shude |last10=Albrow |first10=Michael D. |last11=Chung |first11=Sun-Ju |last12=Han |first12=Cheongho |last13=Jung |first13=Youn Kil |last14=Ryu |first14=Yoon-Hyun |last15=Shin |first15=In-Gu |date=2022-10-01 |title=KMT-2021-BLG-0171Lb and KMT-2021-BLG-1689Lb: two microlensing planets in the KMTNet high-cadence fields with followup observations |url=https://ui.adsabs.harvard.edu/abs/2022MNRAS.516.1894Y |journal=Monthly Notices of the Royal Astronomical Society |volume=516 |issue=2 |pages=1894–1909 |doi=10.1093/mnras/stac2023 |arxiv=2205.12584 |bibcode=2022MNRAS.516.1894Y |issn=0035-8711}}</ref> |2022<ref name=":16">{{Cite journal |last1=Yang |first1=Hongjing |last2=Zang |first2=Weicheng |last3=Gould |first3=Andrew |last4=Yee |first4=Jennifer C. |last5=Hwang |first5=Kyu-Ha |last6=Christie |first6=Grant |last7=Sumi |first7=Takahiro |last8=Zhang |first8=Jiyuan |last9=Mao |first9=Shude |last10=Albrow |first10=Michael D. |last11=Chung |first11=Sun-Ju |last12=Han |first12=Cheongho |last13=Jung |first13=Youn Kil |last14=Ryu |first14=Yoon-Hyun |last15=Shin |first15=In-Gu |date=2022-10-01 |title=KMT-2021-BLG-0171Lb and KMT-2021-BLG-1689Lb: two microlensing planets in the KMTNet high-cadence fields with followup observations |journal=Monthly Notices of the Royal Astronomical Society |volume=516 |issue=2 |pages=1894–1909 |doi=10.1093/mnras/stac2023 |doi-access=free |arxiv=2205.12584 |bibcode=2022MNRAS.516.1894Y |issn=0035-8711}}</ref>
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|KMT-2021-BLG-0119Lb |KMT-2021-BLG-0119Lb
Line 1,050: Line 1,050:
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|2022<ref name=":18">{{Cite journal |last1=Zang |first1=Weicheng |last2=Yang |first2=Hongjing |last3=Han |first3=Cheongho |last4=Lee |first4=Chung-Uk |last5=Udalski |first5=Andrzej |last6=Gould |first6=Andrew |last7=Mao |first7=Shude |last8=Zhang |first8=Xiangyu |last9=Zhu |first9=Wei |last10=Albrow |first10=Michael D. |last11=Chung |first11=Sun-Ju |last12=Hwang |first12=Kyu-Ha |last13=Jung |first13=Youn Kil |last14=Ryu |first14=Yoon-Hyun |last15=Shin |first15=In-Gu |date=2022-09-01 |title=Systematic KMTNet planetary anomaly search. IV. Complete sample of 2019 prime-field |url=https://ui.adsabs.harvard.edu/abs/2022MNRAS.515..928Z |journal=Monthly Notices of the Royal Astronomical Society |volume=515 |issue=1 |pages=928–939 |doi=10.1093/mnras/stac1883 |arxiv=2204.02017 |bibcode=2022MNRAS.515..928Z |issn=0035-8711}}</ref> |2022<ref name=":18">{{Cite journal |last1=Zang |first1=Weicheng |last2=Yang |first2=Hongjing |last3=Han |first3=Cheongho |last4=Lee |first4=Chung-Uk |last5=Udalski |first5=Andrzej |last6=Gould |first6=Andrew |last7=Mao |first7=Shude |last8=Zhang |first8=Xiangyu |last9=Zhu |first9=Wei |last10=Albrow |first10=Michael D. |last11=Chung |first11=Sun-Ju |last12=Hwang |first12=Kyu-Ha |last13=Jung |first13=Youn Kil |last14=Ryu |first14=Yoon-Hyun |last15=Shin |first15=In-Gu |date=2022-09-01 |title=Systematic KMTNet planetary anomaly search. IV. Complete sample of 2019 prime-field |journal=Monthly Notices of the Royal Astronomical Society |volume=515 |issue=1 |pages=928–939 |doi=10.1093/mnras/stac1883 |doi-access=free |arxiv=2204.02017 |bibcode=2022MNRAS.515..928Z |issn=0035-8711}}</ref>
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|KMT-2019-BLG-1552Lb |KMT-2019-BLG-1552Lb
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|2023<ref>{{Cite journal |last1=Zhang |first1=Jiyuan |last2=Zang |first2=Weicheng |last3=Jung |first3=Youn Kil |last4=Yang |first4=Hongjing |last5=Gould |first5=Andrew |last6=Sumi |first6=Takahiro |last7=Mao |first7=Shude |last8=Dong |first8=Subo |last9=Albrow |first9=Michael D. |last10=Chung |first10=Sun-Ju |last11=Han |first11=Cheongho |last12=Hwang |first12=Kyu-Ha |last13=Ryu |first13=Yoon-Hyun |last14=Shin |first14=In-Gu |last15=Shvartzvald |first15=Yossi |date=2023-07-01 |title=KMT-2022-BLG-0440Lb: A new q < 10-4 microlensing planet with the central-resonant caustic degeneracy broken |url=https://ui.adsabs.harvard.edu/abs/2023MNRAS.522.6055Z |journal=Monthly Notices of the Royal Astronomical Society |volume=522 |issue=4 |pages=6055–6069 |doi=10.1093/mnras/stad1398 |arxiv=2301.06779 |bibcode=2023MNRAS.522.6055Z |issn=0035-8711}}</ref> |2023<ref>{{Cite journal |last1=Zhang |first1=Jiyuan |last2=Zang |first2=Weicheng |last3=Jung |first3=Youn Kil |last4=Yang |first4=Hongjing |last5=Gould |first5=Andrew |last6=Sumi |first6=Takahiro |last7=Mao |first7=Shude |last8=Dong |first8=Subo |last9=Albrow |first9=Michael D. |last10=Chung |first10=Sun-Ju |last11=Han |first11=Cheongho |last12=Hwang |first12=Kyu-Ha |last13=Ryu |first13=Yoon-Hyun |last14=Shin |first14=In-Gu |last15=Shvartzvald |first15=Yossi |date=2023-07-01 |title=KMT-2022-BLG-0440Lb: A new q < 10-4 microlensing planet with the central-resonant caustic degeneracy broken |journal=Monthly Notices of the Royal Astronomical Society |volume=522 |issue=4 |pages=6055–6069 |doi=10.1093/mnras/stad1398 |doi-access=free |arxiv=2301.06779 |bibcode=2023MNRAS.522.6055Z |issn=0035-8711}}</ref>
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|KMT-2022-BLG-0371Lb |KMT-2022-BLG-0371Lb
Line 1,362: Line 1,362:
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|2023<ref>{{Cite journal |last1=Specht |first1=D. |last2=Poleski |first2=R. |last3=Penny |first3=M. T. |last4=Kerins |first4=E. |last5=McDonald |first5=I. |last6=Lee |first6=Chung-Uk |last7=Udalski |first7=A. |last8=Bond |first8=I. A. |last9=Shvartzvald |first9=Y. |last10=Zang |first10=Weicheng |last11=Street |first11=R. A. |last12=Hogg |first12=D. W. |last13=Gaudi |first13=B. S. |last14=Barclay |first14=T. |last15=Barentsen |first15=G. |date=2023-04-01 |title=Kepler K2 Campaign 9 - II. First space-based discovery of an exoplanet using microlensing |url=https://ui.adsabs.harvard.edu/abs/2023MNRAS.520.6350S |journal=Monthly Notices of the Royal Astronomical Society |volume=520 |issue=4 |pages=6350–6366 |doi=10.1093/mnras/stad212 |arxiv=2203.16959 |bibcode=2023MNRAS.520.6350S |issn=0035-8711}}</ref> |2023<ref>{{Cite journal |last1=Specht |first1=D. |last2=Poleski |first2=R. |last3=Penny |first3=M. T. |last4=Kerins |first4=E. |last5=McDonald |first5=I. |last6=Lee |first6=Chung-Uk |last7=Udalski |first7=A. |last8=Bond |first8=I. A. |last9=Shvartzvald |first9=Y. |last10=Zang |first10=Weicheng |last11=Street |first11=R. A. |last12=Hogg |first12=D. W. |last13=Gaudi |first13=B. S. |last14=Barclay |first14=T. |last15=Barentsen |first15=G. |date=2023-04-01 |title=Kepler K2 Campaign 9 - II. First space-based discovery of an exoplanet using microlensing |journal=Monthly Notices of the Royal Astronomical Society |volume=520 |issue=4 |pages=6350–6366 |doi=10.1093/mnras/stad212 |doi-access=free |arxiv=2203.16959 |bibcode=2023MNRAS.520.6350S |issn=0035-8711}}</ref>
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|OGLE-2017-BLG-1275Lb |OGLE-2017-BLG-1275Lb
Line 1,494: Line 1,494:
<ref name="Furusawa2013">{{cite journal|title=MOA-2010-BLG-328Lb: A Sub-Neptune Orbiting very Late M Dwarf?|first1=K.|last1=Furusawa|first2=A.|last2=Udalski|first3=T.|last3=Sumi|first4=D. P.|last4=Bennett|first5=I. A.|last5=Bond|first6=A.|last6=Gould|first7=U. G.|last7=Jørgensen|first8=C.|last8=Snodgrass|first9=D. Dominis|last9=Prester|first10=M. D.|last10=Albrow|first11=F.|last11=Abe|first12=C. S.|last12=Botzler|first13=P.|last13=Chote|first14=M.|last14=Freeman|first15=A.|last15=Fukui|first16=P.|last16=Harris|first17=Y.|last17=Itow|first18=C. H.|last18=Ling|first19=K.|last19=Masuda|first20=Y.|last20=Matsubara|first21=N.|last21=Miyake|first22=Y.|last22=Muraki|first23=K.|last23=Ohnishi|first24=N. J.|last24=Rattenbury|first25=To|last25=Saito|first26=D. J.|last26=Sullivan|first27=D.|last27=Suzuki|first28=W. L.|last28=Sweatman|first29=P. J.|last29=Tristram|first30=K.|last30=Wada|first31=P. C. M.|last31=Yock|first32=The MOA|last32=Collaboration|first33=M. K.|last33=Szymański|first34=I.|last34=Soszyński|first35=M.|last35=Kubiak|first36=R.|last36=Poleski|first37=K.|last37=Ulaczyk|first38=G.|last38=Pietrzyński|first39=Ł|last39=Wyrzykowski|first40=The OGLE|last40=Collaboration|first41=J.-Y.|last41=Choi|first42=G. W.|last42=Christie|first43=D. L.|last43=DePoy|first44=Subo|last44=Dong|first45=J.|last45=Drummond|first46=B. S.|last46=Gaudi|first47=C.|last47=Han|last48=L.-W. Hung|first49=K.-H.|last49=Hwang|first50=C.-U.|last50=Lee|first51=J.|last51=McCormick|first52=D.|last52=Moorhouse|first53=T.|last53=Natusch|first54=M.|last54=Nola|first55=E.|last55=Ofek|first56=R. W.|last56=Pogge|last57=I.-G. Shin|first58=J.|last58=Skowron|first59=G.|last59=Thornley|first60=J. C.|last60=Yee|first61=The μFUN|last61=Collaboration|first62=K. A.|last62=Alsubai|first63=V.|last63=Bozza|first64=P.|last64=Browne|first65=M. J.|last65=Burgdorf|first66=S. 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H.|last18=Ling|first19=K.|last19=Masuda|first20=Y.|last20=Matsubara|first21=N.|last21=Miyake|first22=Y.|last22=Muraki|first23=K.|last23=Ohnishi|first24=N. J.|last24=Rattenbury|first25=To|last25=Saito|first26=D. J.|last26=Sullivan|first27=D.|last27=Suzuki|first28=W. L.|last28=Sweatman|first29=P. J.|last29=Tristram|first30=K.|last30=Wada|first31=P. C. M.|last31=Yock|first32=The MOA|last32=Collaboration|first33=M. K.|last33=Szymański|first34=I.|last34=Soszyński|first35=M.|last35=Kubiak|first36=R.|last36=Poleski|first37=K.|last37=Ulaczyk|first38=G.|last38=Pietrzyński|first39=Ł|last39=Wyrzykowski|first40=The OGLE|last40=Collaboration|first41=J.-Y.|last41=Choi|first42=G. W.|last42=Christie|first43=D. L.|last43=DePoy|first44=Subo|last44=Dong|first45=J.|last45=Drummond|first46=B. S.|last46=Gaudi|first47=C.|last47=Han|last48=L.-W. 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Latest revision as of 20:13, 9 December 2024

This article needs to be updated. Please help update this article to reflect recent events or newly available information. (August 2014)

This is a list of exoplanets detected by gravitational microlensing. The phenomenon results in the background star's light being warped around a foreground object, causing a distorted image. If the foreground object is a star with an orbiting planet, we would observe an abnormally bright image. By comparing the luminosity and light distortion of the background star to theoretical models, we can estimate the planet's mass and the distance from its star.

The least massive planet detected by microlensing is KMT-2020-BLG-0414Lb, which has a mass about 1.9 times the mass of earth, or OGLE-2013-BLG-0341LBb, which has a mass about 2 times the mass of earth. The widest separation between a planet and a star is OGLE-2008-BLG-092Lb, which is ~18 AU; the shortest separation is MOA-2015-BLG-337Lb, which is 0.24 AU. There are 7 known multi-planetary systems detected by microlensing, all of which have two planets.

List

Yellow rows denote the members of multi-planet systems. Green rows denote the members of multi-star systems.

Planet Mass (MJ) Projected separation (AU) Period (d) Eccentricity Inclination (°) Year of discovery
OGLE-2003-BLG-235Lb 2.6 5.1 2004
OGLE-2005-BLG-071Lb 3.5 3.6 ~ 3600 2005
OGLE-2005-BLG-390Lb 0.017 2.1 3500 2005
OGLE-2005-BLG-169Lb 0.04 2.8 3300 2006
OGLE-2006-BLG-109Lb 0.727 2.3 1790 64 2008
OGLE-2006-BLG-109Lc 0.271 4.5 4931 0.15 64 2008
MOA-2007-BLG-192Lb 0.01 0.66 2008
MOA-2007-BLG-400Lb 0.9 0.85 2008
MOA-2008-BLG-310Lb 0.23 1.25 2009
OGLE-2007-BLG-368Lb 0.0694 3.3 2009
MOA-2009-BLG-319Lb 0.157 2.0 2010
MOA-2009-BLG-387Lb 2.6 1.8 1970 2011
MOA-2009-BLG-266Lb 0.0327 3.2 2780 2011
MOA-2011-BLG-293Lb 2.4 1.0 2012
MOA-bin-1Lb 3.7 8.3 2012
MOA-2010-BLG-477Lb 1.5 2±1 2012
OGLE-2012-BLG-0026Lb 0.11 3.82 ~3000 2012
OGLE-2012-BLG-0026Lc 0.68 4.63 ~4000 2012
MOA-2010-BLG-073Lb 11 1.21 2012
OGLE-2011-BLG-0251Lb 0.53±0.21 2.72±0.75 or 1.5±0.5 2013
OGLE-2012-BLG-0406Lb 2.73±0.43 3.45±0.26 2013
OGLE-2012-BLG-0358Lb 1.9±0.2 0.87 2013
MOA-2010-BLG-328Lb 0.03 ± 0.0075 0.92 2013
MOA-2011-BLG-322Lb 11.6 4.3 2013
MOA-2008-BLG-379Lb 5±2.5 4±1.6 2013
MOA-2011-BLG-262Lb ~0.053 or ~0.0015 ~0.95 or ~0.13 2013
MOA-2013-BLG-220Lb 2.74 3.03 2014
OGLE-2008-BLG-355Lb 4.6 1.7 2014
OGLE-2013-BLG-0341LBb 0.00522 0.702 2014
OGLE-2013-BLG-0102Lb 13.6 0.8 2014
OGLE-2008-BLG-092Lb 0.137 ~18 2014
OGLE-2014-BLG-0124Lb 0.51±0.16 3.1±0.5 ~2400 2014
OGLE-2011-BLG-0265Lb 1.0 ± 0.3 2 2014
OGLE-2012-BLG-0563Lb 0.39 0.74 2015
OGLE-2015-BLG-0966Lb 0.066 2.7 2015
MOA-2010-BLG-353Lb 0.27 1.72 2015
MOA-2013-BLG-605Lb 0.0102 0.93 2015
MOA-2011-BLG-028Lb 0.09 4.14 2015
OGLE-2015-BLG-0954Lb 3.4 1.6 2016
OGLE-2014-BLG-1760Lb 0.56 1.75 2016
OGLE-2012-BLG-0724Lb 0.47 1.6 2016
OGLE-2015-BLG-0051Lb 0.72 0.73 2016
OGLE-2012-BLG-0950Lb 0.079 2.2 2016
OGLE-2007-BLG-349L(AB)b 0.25 2.59 2557 2016
OGLE-2014-BLG-0676Lb 3.68 4.53 2016
OGLE-2016-BLG-1195Lb 0.0312 2.62 2017
MOA-2012-BLG-505Lb 0.0211 0.9 2017
MOA-2012-BLG-006Lb 8.4 10.2 2017
MOA-2016-BLG-227Lb 2.8 1.39 2017
OGLE-2013-BLG-0132Lb 0.29 3.6 2017
OGLE-2013-BLG-1721Lb 0.64 2.6 2017
OGLE-2016-BLG-0263Lb 4.1 5.4 2017
OGLE-2016-BLG-0613L(AB)b 4.18 6.4 2017
OGLE-2016-BLG-1190Lb 13.38 2.17 1220 0.42 41.2 2017
UKIRT-2017-BLG-001Lb 1.28 4.18 2018
TCP J05074264+2447555b 0.0629 0.940 2018
OGLE-2017-BLG-1522Lb 0.75 0.59 2018
OGLE-2017-BLG-1434Lb 0.014±0.0016 1.18±0.1 2018
OGLE-2017-BLG-1140Lb 1.59 1.02 2018
OGLE-2017-BLG-0482Lb 0.028 1.8 2018
OGLE-2017-BLG-0373Lb 0.401 2.424 2018
OGLE-2017-BLG-0173Lb 0.01029 3.913 2018
OGLE-2014-BLG-1722Lb 0.174 1.5 2018
OGLE-2014-BLG-1722Lc 0.263 1.7 2018
OGLE-2013-BLG-1761Lb 2.7 1.8 2018
OGLE-2011-BLG-0173Lb 0.19 8 2018
MOA-2016-BLG-319Lb 0.62 0.95 2018
MOA-2015-BLG-337Lb 0.106 0.24 2018
MOA-2011-BLG-291Lb 0.057 0.69 2018
MOA-2010-BLG-117Lb 0.54 2.42 2018
KMT-2017-BLG-0165Lb 0.11 3.45 2018
KMT-2016-BLG-2142Lb 15.49 0.83 2018
KMT-2016-BLG-1820Lb 4.57 1.08 2018
KMT-2016-BLG-1397Lb 7.0 5.1 2018
KMT-2016-BLG-0212Lb 18 2.2 2018
OGLE-2018-BLG-1011Lb 1.8 1.8 2019
OGLE-2018-BLG-1011Lc 2.8 0.8 2019
OGLE-2018-BLG-0740Lb 4.8 5.0 5480 0 2019
OGLE-2018-BLG-0596Lb 0.04383 0.97 2019
OGLE-2016-BLG-1067Lb 0.43 1.70 2019
OGLE-2015-BLG-1670Lb 0.0563 2.62 2019
OGLE-2015-BLG-1649Lb 2.54 2.07 2019
OGLE-2013-BLG-0911Lb 9.51 0.39 2019
MOA-bin-29Lb 0.6 0.48 2019
KMT-2018-BLG-1990Lb 0.605 1.083 2019
KMT-2017-BLG-1146Lb 0.71 1.6 2019
KMT-2017-BLG-1038Lb 2.0 1.8 2019
KMT-2016-BLG-1836Lb 2.2 3.5 2019
KMT-2016-BLG-1107Lb 3.283 0.342 2019
OGLE-2018-BLG-1700Lb 4.40 2.8 2020
OGLE-2018-BLG-1269Lb 0.67 4.51 2020
OGLE-2018-BLG-0677Lb 0.0125 0.63 2020
OGLE-2018-BLG-0532Lb 0.01960 1.064 2020
OGLE-2017-BLG-1375Lb 11.28 3.04 2020
OGLE-2017-BLG-1049Lb 5.53 3.92 2020
OGLE-2017-BLG-0604Lb 0.51 4.06 2020
OGLE-2017-BLG-0406Lb 0.41 3.5 2020
OGLE-2016-BLG-1227Lb 0.79 3.4 2020
OGLE-2015-BLG-1771Lb 0.433 0.85 2020
OGLE-2012-BLG-0838Lb 0.167 4.43 2020
OGLE-2006-BLG-284LAb 0.453 2.17 2020
KMT-2019-BLG-1953Lb 0.64 2020
KMT-2019-BLG-1339Lb 1.25 2.15 2020
KMT-2019-BLG-0842Lb 0.03234 3.31 2020
KMT-2018-BLG-1292Lb 4.42 6.03 2020
KMT-2018-BLG-0748Lb 0.19 0.62 2020
KMT-2018-BLG-0029Lb 0.0239 4.27 2020
KMT-2016-BLG-2397Lb 2.63 3.64 2020
KMT-2016-BLG-2364Lb 3.93 2.63 2020
OGLE-2019-BLG-1053Lb 0.00780 3.4 2021
OGLE-2019-BLG-0960Lb 0.0079 1.90 2021
OGLE-2019-BLG-0954Lb 14.2 2.65 2021
OGLE-2019-BLG-0304Lb 0.510 1.23 2021
OGLE-2019-BLG-0299Lb 6.220 2.80 2021
OGLE-2017-BLG-1099Lb 3.02 2.73 2021
OGLE-2018-BLG-1428Lb 0.77 3.30 2021
OGLE-2018-BLG-1185Lb 0.0264 1.54 2021
OGLE-2018-BLG-0962Lb 1.34 3.59 2021
OGLE-2018-BLG-0567Lb 0.32 2.72 2021
KMT-2017-BLG-2509Lb 2.09 2.14 2021
KMT-2018-BLG-1976Lb 2.22 3.54 2021
KMT-2018-BLG-1996Lb 1.09 4.27 2021
KMT-2021-BLG-0322Lb 6.40 2021
KMT-2020-BLG-0414Lb 0.00588 2.07 2021
KMT-2020-BLG-0414Lc 27 22.3 2021
KMT-2019-BLG-1715Lb 2.56 3.32 2021
KMT-2019-BLG-0371Lb 7.7 0.79 2021
KMT-2018-BLG-1743Lb 0.245 1.449 2021
KMT-2018-BLG-1025Lb 0.019064 1.305 2021
KMT-2016-BLG-2605Lb 0.7710 0.681 2021
OGLE-2019-BLG-1470L(AB)c 2.2 3.2 2022
OGLE-2019-BLG-1492Lb 0.117 2.7 2022
OGLE-2018-BLG-0977Lb 0.0201 2.0 2022
OGLE-2018-BLG-0516Lb 0.0632 2.2 2022
OGLE-2018-BLG-0506Lb 0.0513 3.0 2022
OGLE-2019-BLG-0468Lb 3.43 3.29 2022
OGLE-2019-BLG-0468Lc 10.22 2.77 2022
OGLE-2019-BLG-0362Lb 3.26 2.18 2022
OGLE-2018-BLG-1647Lb 0.970 1.36 2022
OGLE-2018-BLG-1367Lb 0.950 1.21 2022
OGLE-2018-BLG-1126Lb 0.056 3.23 2022
OGLE-2018-BLG-1119Lb 0.910 4.06 2022
OGLE-2018-BLG-0298Lb 0.14 2.86 2022
OGLE-2018-BLG-0383Lb 0.0201 1.8 2022
OGLE-2017-BLG-1691Lb 0.046 2.41 2022
OGLE-2018-BLG-0799Lb 0.26 1.28 2022
OGLE-2018-BLG-0932Lb 0.890 1.75 2022
OGLE-2018-BLG-1212Lb 0.20 1.68 2022
OGLE-2016-BLG-1093Lb 0.71 2.13 2022
OGLE-2014-BLG-0319Lb 0.57 3.49 2022
MOA-2020-BLG-135Lb 0.0356 1.11 2022
MOA-2019-BLG-008Lb 18 2022
KMT-2019-BLG-0253Lb 0.0488 1.1 2022
KMT-2021-BLG-2294Lb 0.070 1.15 2022
KMT-2021-BLG-1898Lb 0.730 1.9 2022
KMT-2021-BLG-1689Lb 0.14 2.5 2022
KMT-2021-BLG-0119Lb 5.52 2.92 2022
KMT-2021-BLG-0192Lb 0.11 1.62 2022
KMT-2021-BLG-0171Lb 0.0352 3.5 2022
KMT-2021-BLG-1303Lb 0.38 2.89 2022
KMT-2021-BLG-0320Lb 0.10 1.54 2022
KMT-2021-BLG-1554Lb 0.12 0.72 2022
KMT-2021-BLG-1391Lb 0.0143 2.29 2022
KMT-2021-BLG-1372Lb 0.1928 2.37 2022
KMT-2021-BLG-1253Lb 0.05994 1.52 2022
KMT-2019-BLG-0953Lb 0.0289 3.1 2022
KMT-2021-BLG-0748Lb 0.45 2.43 2022
KMT-2021-BLG-1077Lb 0.22 1.26 2022
KMT-2021-BLG-1077Lc 0.25 0.930 2022
KMT-2021-BLG-0912Lb 0.00884 3.14 2022
KMT-2021-BLG-0240Lb 0.21 2.8 2022
KMT-2021-BLG-2974Lb 0.28 2.0 2022
KMT-2019-BLG-1552Lb 4.05 2.6 2022
KMT-2019-BLG-1042Lb 0.19 1.7 2022
KMT-2018-BLG-1988Lb 0.0175 3.09 2022
KMT-2019-BLG-0414Lb 4.57 1.16 2022
KMT-2017-BLG-0673Lb 3.67 2.34 2022
KMT-2018-BLG-0087Lb 0.23 0.870 2022
KMT-2018-BLG-0030Lb 1.45 4.39 2022
KMT-2018-BLG-0247Lb 2.11 2.46 2022
KMT-2018-BLG-2602Lb 1.15 3.81 2022
OGLE-2019-BLG-1180Lb 1.747 5.19 2023
OGLE-2019-BLG-0679Lb 3.34 6.99 2023
OGLE-2019-BLG-0249Lb 7.12 1.84 2023
OGLE-2017-BLG-1806Lb 0.0166 1.75 2023
MOA-2022-BLG-249Lb 0.0152 1.63 2023
MOA-2020-BLG-208Lb 0.14 2.74 2023
KMT-2022-BLG-1013Lb 0.31 1.38 2023
KMT-2022-BLG-0440Lb 0.0485 1.9 2023
KMT-2022-BLG-0371Lb 0.26 3.02 2023
KMT-2021-BLG-2478Lb 0.900 1.85 2023
KMT-2021-BLG-2010Lb 1.07 1.79 2023
KMT-2021-BLG-1770Lb 21 0.900 2023
KMT-2021-BLG-1547Lb 1.47 4.5 2023
KMT-2021-BLG-1150Lb 0.880 4.5 2023
KMT-2021-BLG-1105Lb 1.30 3.54 2023
KMT-2021-BLG-0909Lb 1.26 1.75 2023
KMT-2021-BLG-0712Lb 0.1202 2.22 2023
KMT-2019-BLG-2783Lb 1.16 1.85 2023
KMT-2019-BLG-1806Lb 0.0147 3.02 2023
KMT-2019-BLG-1367Lb 0.0128 1.70 2023
KMT-2019-BLG-1216Lb 0.0940 2.44 2023
KMT-2019-BLG-0335Lb 21 1.64 2023
KMT-2019-BLG-0298Lb 1.81 5.67 2023
KMT-2019-BLG-0297Lb 19 0.960 2023
KMT-2018-BLG-0885Lb 29 1.07 2023
KMT-2017-BLG-1194Lb 0.0111 1.78 2023
KMT-2017-BLG-1003Lb 0.01633 1.38 2023
KMT-2017-BLG-0428Lb 0.0176 1.81 2023
KMT-2016-BLG-1105Lb 0.00730 2.44 2023
K2-2016-BLG-0005Lb 1.10 4.16 4700 2023
OGLE-2017-BLG-1275Lb 5.90 2.09 2024
OGLE-2017-BLG-1237Lb 3.80 2.53 2024
OGLE-2017-BLG-0640Lb 1.62 1.14 2024

Candidate rogue planets

A number of candidate rogue planets have been detected by microlensing.

Planet Mass Year of discovery
MOA-2011-BLG-274L 0.8±0.3 MJ 2014
OGLE-2016-BLG-1540L ~35 M🜨 2017
OGLE-2012-BLG-1323L ~2.3 M🜨 2018
OGLE-2017-BLG-0560L ~1.9 MJ 2018
OGLE-2019-BLG-0551L ~7.7 M🜨 2020
KMT-2019-BLG-2073L ~59 M🜨 2020
OGLE-2016-BLG-1928L ~0.3 M🜨 2020
KMT-2017-BLG-2820L ~8.2 M🜨 2020

Unconfirmed detections

Some microlensing events, such as MACHO-98-BLG-35 and PA-99-N2, suggest the possible presence of a planetary companion to the lensing star, but this is unconfirmed. Since microlensing relies on a one-time chance alignment, it is likely not possible to confirm these detections.

In some cases, a planetary interpretation for a microlensing event was proposed, but has been disproven. MACHO-1997-BLG-41 was initially interpreted as a binary star system orbited by a circumbinary planet, but a different model with two stars and no planet was later found to be a better fit to the data. Similarly, OGLE-2013-BLG-0723L was initially interpreted as a binary system of a star and a brown dwarf, with a low-mass planet orbiting the brown dwarf, but a model where the system consists of two low-mass stars with no planet was found to be a better fit to the data.

See also

Notes

  1. The nature of the observed system is unclear. It is either a rogue planet with about 3.2 MJ masses and a 0.5 ME exomoon or a red dwarf with 18 ME planet.

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