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| UKIRT-2017-BLG-001Lb || 1.28 || 4.18 || || || || 2018<ref>{{Cite journal |last=Shvartzvald |first=Y. |last2=Calchi Novati |first2=S. |last3=Gaudi |first3=B. S. |last4=Bryden |first4=G. |last5=Nataf |first5=D. M. |last6=Penny |first6=M. T. |last7=Beichman |first7=C. |last8=Henderson |first8=C. B. |last9=Jacklin |first9=S. |last10=Schlafly |first10=E. F. |last11=Huston |first11=M. J. |date=2018-04-01 |title=UKIRT-2017-BLG-001Lb: A Giant Planet Detected through the Dust |url=https://ui.adsabs.harvard.edu/abs/2018ApJ...857L...8S |journal=The Astrophysical Journal |volume=857 |pages=L8 |doi=10.3847/2041-8213/aab71b |issn=0004-637X}}</ref>
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|2018<ref>{{Cite journal |last=Nucita |first=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 |pages=2962–2967 |doi=10.1093/mnras/sty448 |issn=0035-8711}}</ref><ref>{{Cite journal |last=Zang |first=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 |url=https://ui.adsabs.harvard.edu/abs/2020ApJ...897..180Z |journal=The Astrophysical Journal |volume=897 |pages=180 |doi=10.3847/1538-4357/ab9749 |issn=0004-637X}}</ref><ref>{{Cite journal |last=Fukui |first=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 |url=https://ui.adsabs.harvard.edu/abs/2019AJ....158..206F |journal=The Astronomical Journal |volume=158 |pages=206 |doi=10.3847/1538-3881/ab487f |issn=0004-6256}}</ref>
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|2018<ref>{{Cite journal |last=Jung |first=Y. K. |last2=Udalski |first2=A. |last3=Gould |first3=A. |last4=Ryu |first4=Y. -H. |last5=Yee |first5=J. C. |last6=and |last7=Han |first7=C. |last8=Albrow |first8=M. D. |last9=Lee |first9=C. -U. |last10=Kim |first10=S. -L. |last11=Hwang |first11=K. -H. |last12=Chung |first12=S. -J. |last13=Shin |first13=I. -G. |last14=Zhu |first14=W. |last15=Cha |first15=S. -M. |date=2018-05-01 |title=OGLE-2017-BLG-1522: A Giant Planet around a Brown Dwarf Located in the Galactic Bulge |url=https://ui.adsabs.harvard.edu/abs/2018AJ....155..219J |journal=The Astronomical Journal |volume=155 |pages=219 |doi=10.3847/1538-3881/aabb51 |issn=0004-6256}}</ref>
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|2018{{Cite journal |arxiv=1802.02582 |doi=10.32023/0001-5237/68.1.1 |date=2018 |volume=68 |issue=1 |last1=Udalski |first1=A. |last2=Ryu |first2=Y.-H. |last3=Sajadian |first3=S. |last4=Gould |first4=A. |last5=Mróz |first5=P. |last6=Poleski |first6=R. |last7=Szymański |first7=M.K. |last8=Skowron |first8=J. |last9=Soszyński |first9=I. |last10=Kozłowski |first10=S. |last11=Pietrukowicz |first11=P. |last12=Ulaczyk |first12=K. |last13=Pawlak |first13=M. |last14=Rybicki |first14=K. |last15=Iwanek |first15=P. |last16=Albrow |first16=M.D. |last17=Chung |first17=S.-J. |last18=Han |first18=C. |last19=Hwang |first19=K.-H. |last20=Jung |first20=Y.K. |last21=Shin |first21=I.-G. |last22=Shvartzvald |first22=Y. |last23=Yee |first23=J.C. |last24=Zang |first24=W. |last25=Zhu |first25=W. |last26=Cha |first26=S.-M. |last27=Kim |first27=D.-J. |last28=Kim |first28=H.-W. |last29=Kim |first29=S.-L. |last30=Lee |first30=C.-U. |title=OGLE-2017-BLG-1434Lb: Eighth q<1×10<sup>-4</sup> Mass-Ratio Microlens Planet Confirms Turnover in Planet Mass-Ratio Function |journal=Acta Astronomica |s2cid=119011208 |display-authors=1 }} |2018<ref>{{Cite journal |last=Udalski |first=A. |last2=Ryu |first2=Y.-H. |last3=Sajadian |first3=S. |last4=Gould |first4=A. |last5=Mróz |first5=P. |last6=Poleski |first6=R. |last7=Szymański |first7=M.K. |last8=Skowron |first8=J. |last9=Soszyński |first9=I. |last10=Kozłowski |first10=S. |last11=Pietrukowicz |first11=P. |last12=Ulaczyk |first12=K. |last13=Pawlak |first13=M. |last14=Rybicki |first14=K. |last15=Iwanek |first15=P. |date=March 2018 |title=OGLE-2017-BLG-1434Lb: Eighth q |url=https://doi.org/10.32023/0001-5237/68.1.1 |journal=Acta Astronomica |volume=68 |issue=1 |pages=1–42 |doi=10.32023/0001-5237/68.1.1}}</ref>
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|2018<ref>{{Cite journal |last=Calchi Novati |first=S. |last2=Skowron |first2=J. |last3=Jung |first3=Y. K. |last4=Beichman |first4=C. |last5=Bryden |first5=G. |last6=Carey |first6=S. |last7=Gaudi |first7=B. S. |last8=Henderson |first8=C. B. |last9=Shvartzvald |first9=Y. |last10=Yee |first10=J. C. |last11=Zhu |first11=W. |last12=Spitzer Team |last13=Udalski |first13=A. |last14=Szymański |first14=M. K. |last15=Mróz |first15=P. |date=2018-06-01 |title=Spitzer Opens New Path to Break Classic Degeneracy for Jupiter-mass Microlensing Planet OGLE-2017-BLG-1140Lb |url=https://ui.adsabs.harvard.edu/abs/2018AJ....155..261C |journal=The Astronomical Journal |volume=155 |pages=261 |doi=10.3847/1538-3881/aac21c |issn=0004-6256}}</ref>
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|2018<ref>{{Cite journal |last=Han |first=C. |last2=Hirao |first2=Y. |last3=Udalski |first3=A. |last4=Lee |first4=C. -U. |last5=Bozza |first5=V. |last6=Gould |first6=A. |last7=and |last8=Abe |first8=F. |last9=Barry |first9=R. |last10=Bond |first10=I. A. |last11=Bennett |first11=D. P. |last12=Bhattacharya |first12=A. |last13=Donachie |first13=M. |last14=Evans |first14=P. |last15=Fukui |first15=A. |date=2018-05-01 |title=OGLE-2017-BLG-0482Lb: A Microlensing Super-Earth Orbiting a Low-mass Host Star |url=https://ui.adsabs.harvard.edu/abs/2018AJ....155..211H |journal=The Astronomical Journal |volume=155 |pages=211 |doi=10.3847/1538-3881/aabad2 |issn=0004-6256}}</ref>
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|2018<ref>{{Cite journal |last=Skowron |first=J. |last2=Ryu |first2=Y. -H. |last3=Hwang |first3=K. -H. |last4=Udalski |first4=A. |last5=Mróz |first5=P. |last6=Kozłowski |first6=S. |last7=Soszyński |first7=I. |last8=Pietrukowicz |first8=P. |last9=Szymański |first9=M. K. |last10=Poleski |first10=R. |last11=Ulaczyk |first11=K. |last12=Pawlak |first12=M. |last13=Rybicki |first13=K. |last14=Iwanek |first14=P. |last15=Albrow |first15=M. D. |date=2018-03-01 |title=OGLE-2017-BLG-0373Lb: A Jovian Mass-Ratio Planet Exposes A New Accidental Microlensing Degeneracy |url=https://ui.adsabs.harvard.edu/abs/2018AcA....68...43S |journal=Acta Astronomica |volume=68 |pages=43–61 |doi=10.32023/0001-5237/68.1.2 |issn=0001-5237}}</ref>
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|2018<ref>{{Cite journal |last=Hwang |first=K. -H. |last2=Udalski |first2=A. |last3=Shvartzvald |first3=Y. |last4=Ryu |first4=Y. -H. |last5=Albrow |first5=M. D. |last6=Chung |first6=S. -J. |last7=Gould |first7=A. |last8=Han |first8=C. |last9=Jung |first9=Y. K. |last10=Shin |first10=I. -G. |last11=Yee |first11=J. C. |last12=Zhu |first12=W. |last13=Cha |first13=S. -M. |last14=Kim |first14=D. -J. |last15=Kim |first15=H. -W. |date=2018-01-01 |title=OGLE-2017-BLG-0173Lb: Low-mass-ratio Planet in a “Hollywood” Microlensing Event |url=https://ui.adsabs.harvard.edu/abs/2018AJ....155...20H |journal=The Astronomical Journal |volume=155 |pages=20 |doi=10.3847/1538-3881/aa992f |issn=0004-6256}}</ref>
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|2018<ref name=":0">{{Cite journal |last=Suzuki |first=D. |last2=Bennett |first2=D. P. |last3=Udalski |first3=A. |last4=Bond |first4=I. A. |last5=Sumi |first5=T. |last6=Han |first6=C. |last7=Kim |first7=Ho-il. |last8=Abe |first8=F. |last9=Asakura |first9=Y. |last10=Barry |first10=R. K. |last11=Bhattacharya |first11=A. |last12=Donachie |first12=M. |last13=Freeman |first13=M. |last14=Fukui |first14=A. |last15=Hirao |first15=Y. |date=2018-06-01 |title=A Likely Detection of a Two-planet System in a Low-magnification Microlensing Event |url=https://ui.adsabs.harvard.edu/abs/2018AJ....155..263S |journal=The Astronomical Journal |volume=155 |pages=263 |doi=10.3847/1538-3881/aabd7a |issn=0004-6256}}</ref>
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| MOA-bin-29Lb || 0.6 || 0.48 || || || || 2019<ref name="Kondo2019"/> | MOA-bin-29Lb || 0.6 || 0.48 || || || || 2019<ref name="Kondo2019"/>
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|2021{{Cite journal |arxiv=2103.01896 |doi=10.1088/1674-4527/21/9/239 |title=An Earth-mass planet in a time of COVID-19: KMT-2020-BLG-0414Lb |date=2021 |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 |last16=Shin |first16=In-Gu |last17=Cha |first17=Sang-Mok |last18=Kim |first18=Dong-Jin |last19=Kim |first19=Hyoun-Woo |last20=Kim |first20=Seung-Lee |last21=Lee |first21=Dong-Joo |last22=Lee |first22=Yongseok |last23=Park |first23=Byeong-Gon |last24=Pogge |first24=Richard W. |last25=Drummond |first25=John |last26=Tan |first26=Thiam-Guan |last27=Nascimento Júnior |first27=José Dias do |last28=Maoz |first28=Dan |last29=Penny |first29=Matthew T. |last30=Zhu |first30=Wei |journal=Research in Astronomy and Astrophysics |volume=21 |issue=9 |page=239 |display-authors=1 }} |2021<ref>{{Cite journal |last=Zang |first=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 |issn=1674-4527}}</ref>
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| KMT-2019-BLG-0371Lb || 7.7 || 0.79 || || || || 2021<ref name="Kim2021"/> | KMT-2019-BLG-0371Lb || 7.7 || 0.79 || || || || 2021<ref name="Kim2021"/>

Revision as of 00:45, 17 April 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 about the same mass as Earth. The widest separation between a planet and a star is OGLE-2008-BLG-092Lb, which is ~15 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.

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)c 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
MOA-bin-29Lb 0.6 0.48 2019
KMT-2020-BLG-0414Lb 0.00381 1.79 2021
KMT-2019-BLG-0371Lb 7.7 0.79 2021

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.

References

  1. "Planetary Systems Composite Data". NASA Exoplanet Archive. Retrieved 19 February 2023.
  2. Bond, I. A.; et al. (2004). "OGLE 2003-BLG-235/MOA 2003-BLG-53: A Planetary Microlensing Event". The Astrophysical Journal. 606 (2): L155 – L158. arXiv:astro-ph/0404309. Bibcode:2004ApJ...606L.155B. doi:10.1086/420928. S2CID 17610640.
  3. Bennett, David P.; et al. (2006). "Identification of the OGLE-2003-BLG-235/MOA-2003-BLG-53 Planetary Host Star". The Astrophysical Journal Letters. 647 (2): L171 – L174. arXiv:astro-ph/0606038. Bibcode:2006ApJ...647L.171B. doi:10.1086/507585. S2CID 11294425.
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