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List of exoplanets detected by microlensing

(Redirected from List of extrasolar planets detected by microlensing)

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.[1][2] 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.[3]

List

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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[4][5]
OGLE-2005-BLG-071Lb 3.5 3.6 ~ 3600 2005[6][7]
OGLE-2005-BLG-390Lb 0.017 2.1 3500 2005[8]
OGLE-2005-BLG-169Lb 0.04 2.8 3300 2006[9]
OGLE-2006-BLG-109Lb 0.727 2.3 1790 64 2008[10]
OGLE-2006-BLG-109Lc 0.271 4.5 4931 0.15 64 2008[10]
MOA-2007-BLG-192Lb 0.01 0.66 2008[11]
MOA-2007-BLG-400Lb 0.9 0.85 2008[12]
MOA-2008-BLG-310Lb 0.23 1.25 2009[13]
OGLE-2007-BLG-368Lb 0.0694 3.3 2009[14]
MOA-2009-BLG-319Lb 0.157 2.0 2010[15]
MOA-2009-BLG-387Lb 2.6 1.8 1970 2011[16]
MOA-2009-BLG-266Lb 0.0327 3.2 2780 2011[17]
MOA-2011-BLG-293Lb 2.4 1.0 2012[18]
MOA-bin-1Lb 3.7 8.3 2012[19]
MOA-2010-BLG-477Lb 1.5 2±1 2012[20]
OGLE-2012-BLG-0026Lb 0.11 3.82 ~3000 2012[21]
OGLE-2012-BLG-0026Lc 0.68 4.63 ~4000 2012[21]
MOA-2010-BLG-073Lb 11 1.21 2012[22]
OGLE-2011-BLG-0251Lb 0.53±0.21 2.72±0.75 or 1.5±0.5 2013[23]
OGLE-2012-BLG-0406Lb 2.73±0.43 3.45±0.26 2013[24]
OGLE-2012-BLG-0358Lb 1.9±0.2 0.87 2013[25]
MOA-2010-BLG-328Lb 0.03 ± 0.0075 0.92 2013[26]
MOA-2011-BLG-322Lb 11.6 4.3 2013[27]
MOA-2008-BLG-379Lb 5±2.5 4±1.6 2013[28]
MOA-2011-BLG-262Lb[note 1] ~0.053 or ~0.0015 ~0.95 or ~0.13 2013[29]
MOA-2013-BLG-220Lb 2.74 3.03 2014[30][31]
OGLE-2008-BLG-355Lb 4.6 1.7 2014[32]
OGLE-2013-BLG-0341LBb 0.00522 0.702 2014[2]
OGLE-2013-BLG-0102Lb 13.6 0.8 2014[33]
OGLE-2008-BLG-092Lb 0.137 ~18 2014[34]
OGLE-2014-BLG-0124Lb 0.51±0.16 3.1±0.5 ~2400 2014[35]
OGLE-2011-BLG-0265Lb 1.0 ± 0.3 2 2014[36]
OGLE-2012-BLG-0563Lb 0.39 0.74 2015[37]
OGLE-2015-BLG-0966Lb 0.066 2.7 2015[38]
MOA-2010-BLG-353Lb 0.27 1.72 2015[39]
MOA-2013-BLG-605Lb 0.0102 0.93 2015[40]
MOA-2011-BLG-028Lb 0.09 4.14 2015[41]
OGLE-2015-BLG-0954Lb 3.4 1.6 2016[42]
OGLE-2014-BLG-1760Lb 0.56 1.75 2016[43]
OGLE-2012-BLG-0724Lb 0.47 1.6 2016[44]
OGLE-2015-BLG-0051Lb 0.72 0.73 2016[45]
OGLE-2012-BLG-0950Lb 0.079 2.2 2016[46]
OGLE-2007-BLG-349L(AB)c 0.25 2.59 2557 2016[47]
OGLE-2014-BLG-0676Lb 3.68 4.53 2016[48]
OGLE-2016-BLG-1195Lb 0.0312 2.62 2017[49][50]
MOA-2012-BLG-505Lb 0.0211 0.9 2017[51]
MOA-2012-BLG-006Lb 8.4 10.2 2017[52]
MOA-2016-BLG-227Lb 2.8 1.39 2017[53]
OGLE-2013-BLG-0132Lb 0.29 3.6 2017[54]
OGLE-2013-BLG-1721Lb 0.64 2.6 2017[54]
OGLE-2016-BLG-0263Lb 4.1 5.4 2017[55]
OGLE-2016-BLG-0613L(AB)b 4.18 6.4 2017[56]
OGLE-2016-BLG-1190Lb 13.38 2.17 1220 0.42 41.2 2017[57]
UKIRT-2017-BLG-001Lb 1.28 4.18 2018[58]
TCP J05074264+2447555b 0.0629 0.940 2018[59][60][61]
OGLE-2017-BLG-1522Lb 0.75 0.59 2018[62]
OGLE-2017-BLG-1434Lb 0.014±0.0016 1.18±0.1 2018[63]
OGLE-2017-BLG-1140Lb 1.59 1.02 2018[64]
OGLE-2017-BLG-0482Lb 0.028 1.8 2018[65]
OGLE-2017-BLG-0373Lb 0.401 2.424 2018[66]
OGLE-2017-BLG-0173Lb 0.01029 3.913 2018[67]
OGLE-2014-BLG-1722Lb 0.174 1.5 2018[68]
OGLE-2014-BLG-1722Lc 0.263 1.7 2018[68]
OGLE-2013-BLG-1761Lb 2.7 1.8 2018[69]
OGLE-2011-BLG-0173Lb 0.19 8 2018[70]
MOA-2016-BLG-319Lb 0.62 0.95 2018[71]
MOA-2015-BLG-337Lb 0.106 0.24 2018[72]
MOA-2011-BLG-291Lb 0.057 0.69 2018[73]
MOA-2010-BLG-117Lb 0.54 2.42 2018[74]
KMT-2017-BLG-0165Lb 0.11 3.45 2018[75]
KMT-2016-BLG-2142Lb 15.49 0.83 2018[76]
KMT-2016-BLG-1820Lb 4.57 1.08 2018[76]
KMT-2016-BLG-1397Lb 7.0 5.1 2018[77]
KMT-2016-BLG-0212Lb 18 2.2 2018[78]
OGLE-2018-BLG-1011Lb 1.8 1.8 2019[79]
OGLE-2018-BLG-1011Lc 2.8 0.8 2019[79]
OGLE-2018-BLG-0740Lb 4.8 5.0 5480 0 2019[80]
OGLE-2018-BLG-0596Lb 0.04383 0.97 2019[81]
OGLE-2016-BLG-1067Lb 0.43 1.70 2019[82]
OGLE-2015-BLG-1670Lb 0.0563 2.62 2019[83]
OGLE-2015-BLG-1649Lb 2.54 2.07 2019[84]
OGLE-2013-BLG-0911Lb 9.51 0.39 2019[85]
MOA-bin-29Lb 0.6 0.48 2019[86]
KMT-2018-BLG-1990Lb 0.605 1.083 2019[87]
KMT-2017-BLG-1146Lb 0.71 1.6 2019[88]
KMT-2017-BLG-1038Lb 2.0 1.8 2019[88]
KMT-2016-BLG-1836Lb 2.2 3.5 2019[89]
KMT-2016-BLG-1107Lb 3.283 0.342 2019[90]
OGLE-2018-BLG-1700Lb 4.40 2.8 2020[91]
OGLE-2018-BLG-1269Lb 0.67 4.51 2020[92]
OGLE-2018-BLG-0677Lb 0.0125 0.63 2020[93]
OGLE-2018-BLG-0532Lb 0.01960 1.064 2020[94]
OGLE-2017-BLG-1375Lb 11.28 3.04 2020[95]
OGLE-2017-BLG-1049Lb 5.53 3.92 2020[96]
OGLE-2017-BLG-0604Lb 0.51 4.06 2020[95]
OGLE-2017-BLG-0406Lb 0.41 3.5 2020[97]
OGLE-2016-BLG-1227Lb 0.79 3.4 2020[98]
OGLE-2015-BLG-1771Lb 0.433 0.85 2020[99]
OGLE-2012-BLG-0838Lb 0.167 4.43 2020[100]
OGLE-2006-BLG-284LAb 0.453 2.17 2020[101]
KMT-2019-BLG-1953Lb 0.64 2020[102]
KMT-2019-BLG-1339Lb 1.25 2.15 2020[103]
KMT-2019-BLG-0842Lb 0.03234 3.31 2020[104]
KMT-2018-BLG-1292Lb 4.42 6.03 2020[105]
KMT-2018-BLG-0748Lb 0.19 0.62 2020[106]
KMT-2018-BLG-0029Lb 0.0239 4.27 2020[107]
KMT-2016-BLG-2397Lb 2.63 3.64 2020[95]
KMT-2016-BLG-2364Lb 3.93 2.63 2020[95]
OGLE-2019-BLG-1053Lb 0.00780 3.4 2021[108]
OGLE-2019-BLG-0960Lb 0.0079 1.90 2021[109]
OGLE-2019-BLG-0954Lb 14.2 2.65 2021[110]
OGLE-2019-BLG-0304Lb 0.510 1.23 2021[111]
OGLE-2019-BLG-0299Lb 6.220 2.80 2021[112]
OGLE-2017-BLG-1099Lb 3.02 2.73 2021[112]
OGLE-2018-BLG-1428Lb 0.77 3.30 2021[113]
OGLE-2018-BLG-1185Lb 0.0264 1.54 2021[114]
OGLE-2018-BLG-0962Lb 1.34 3.59 2021[115]
OGLE-2018-BLG-0567Lb 0.32 2.72 2021[115]
KMT-2017-BLG-2509Lb 2.09 2.14 2021[112]
KMT-2018-BLG-1976Lb 2.22 3.54 2021[110]
KMT-2018-BLG-1996Lb 1.09 4.27 2021[110]
KMT-2021-BLG-0322Lb 6.40 2021[116]
KMT-2020-BLG-0414Lb 0.00588 2.07 2021[117][1]
KMT-2020-BLG-0414Lc 27 22.3 2021[117][1]
KMT-2019-BLG-1715Lb 2.56 3.32 2021[118]
KMT-2019-BLG-0371Lb 7.7 0.79 2021[119]
KMT-2018-BLG-1743Lb 0.245 1.449 2021[120]
KMT-2018-BLG-1025Lb 0.019064 1.305 2021[121]
KMT-2016-BLG-2605Lb 0.7710 0.681 2021[122]
OGLE-2019-BLG-1470L(AB)c 2.2 3.2 2022[123]
OGLE-2019-BLG-1492Lb 0.117 2.7 2022[124]
OGLE-2018-BLG-0977Lb 0.0201 2.0 2022[124]
OGLE-2018-BLG-0516Lb 0.0632 2.2 2022[124]
OGLE-2018-BLG-0506Lb 0.0513 3.0 2022[124]
OGLE-2019-BLG-0468Lb 3.43 3.29 2022[125]
OGLE-2019-BLG-0468Lc 10.22 2.77 2022[125]
OGLE-2019-BLG-0362Lb 3.26 2.18 2022[126]
OGLE-2018-BLG-1647Lb 0.970 1.36 2022[127]
OGLE-2018-BLG-1367Lb 0.950 1.21 2022[127]
OGLE-2018-BLG-1126Lb 0.056 3.23 2022[127]
OGLE-2018-BLG-1119Lb 0.910 4.06 2022[128]
OGLE-2018-BLG-0298Lb 0.14 2.86 2022[128]
OGLE-2018-BLG-0383Lb 0.0201 1.8 2022[129]
OGLE-2017-BLG-1691Lb 0.046 2.41 2022[130]
OGLE-2018-BLG-0799Lb 0.26 1.28 2022[131]
OGLE-2018-BLG-0932Lb 0.890 1.75 2022[127]
OGLE-2018-BLG-1212Lb 0.20 1.68 2022[127]
OGLE-2016-BLG-1093Lb 0.71 2.13 2022[132]
OGLE-2014-BLG-0319Lb 0.57 3.49 2022[133]
MOA-2020-BLG-135Lb 0.0356 1.11 2022[134]
MOA-2019-BLG-008Lb 18 2022[135]
KMT-2019-BLG-0253Lb 0.0488 1.1 2022[124]
KMT-2021-BLG-2294Lb 0.070 1.15 2022[136]
KMT-2021-BLG-1898Lb 0.730 1.9 2022[137]
KMT-2021-BLG-1689Lb 0.14 2.5 2022[138]
KMT-2021-BLG-0119Lb 5.52 2.92 2022[136]
KMT-2021-BLG-0192Lb 0.11 1.62 2022[136]
KMT-2021-BLG-0171Lb 0.0352 3.5 2022[138]
KMT-2021-BLG-1303Lb 0.38 2.89 2022[130]
KMT-2021-BLG-0320Lb 0.10 1.54 2022[130]
KMT-2021-BLG-1554Lb 0.12 0.72 2022[130]
KMT-2021-BLG-1391Lb 0.0143 2.29 2022[139]
KMT-2021-BLG-1372Lb 0.1928 2.37 2022[139]
KMT-2021-BLG-1253Lb 0.05994 1.52 2022[139]
KMT-2019-BLG-0953Lb 0.0289 3.1 2022[124]
KMT-2021-BLG-0748Lb 0.45 2.43 2022[139]
KMT-2021-BLG-1077Lb 0.22 1.26 2022[140]
KMT-2021-BLG-1077Lc 0.25 0.930 2022[140]
KMT-2021-BLG-0912Lb 0.00884 3.14 2022[141]
KMT-2021-BLG-0240Lb 0.21 2.8 2022[142]
KMT-2021-BLG-2974Lb 0.28 2.0 2022[143]
KMT-2019-BLG-1552Lb 4.05 2.6 2022[143]
KMT-2019-BLG-1042Lb 0.19 1.7 2022[143]
KMT-2018-BLG-1988Lb 0.0175 3.09 2022[144]
KMT-2019-BLG-0414Lb 4.57 1.16 2022[145]
KMT-2017-BLG-0673Lb 3.67 2.34 2022[145]
KMT-2018-BLG-0087Lb 0.23 0.870 2022[128]
KMT-2018-BLG-0030Lb 1.45 4.39 2022[128]
KMT-2018-BLG-0247Lb 2.11 2.46 2022[128]
KMT-2018-BLG-2602Lb 1.15 3.81 2022[128]
OGLE-2019-BLG-1180Lb 1.747 5.19 2023[146]
OGLE-2019-BLG-0679Lb 3.34 6.99 2023[147]
OGLE-2019-BLG-0249Lb 7.12 1.84 2023[147]
OGLE-2017-BLG-1806Lb 0.0166 1.75 2023[148]
MOA-2022-BLG-249Lb 0.0152 1.63 2023[149]
MOA-2020-BLG-208Lb 0.14 2.74 2023[150]
KMT-2022-BLG-1013Lb 0.31 1.38 2023[151]
KMT-2022-BLG-0440Lb 0.0485 1.9 2023[152]
KMT-2022-BLG-0371Lb 0.26 3.02 2023[151]
KMT-2021-BLG-2478Lb 0.900 1.85 2023[153]
KMT-2021-BLG-2010Lb 1.07 1.79 2023[154]
KMT-2021-BLG-1770Lb 21 0.900 2023[155]
KMT-2021-BLG-1547Lb 1.47 4.5 2023[156]
KMT-2021-BLG-1150Lb 0.880 4.5 2023[157]
KMT-2021-BLG-1105Lb 1.30 3.54 2023[153]
KMT-2021-BLG-0909Lb 1.26 1.75 2023[153]
KMT-2021-BLG-0712Lb 0.1202 2.22 2023[153]
KMT-2019-BLG-2783Lb 1.16 1.85 2023[147]
KMT-2019-BLG-1806Lb 0.0147 3.02 2023[148]
KMT-2019-BLG-1367Lb 0.0128 1.70 2023[148]
KMT-2019-BLG-1216Lb 0.0940 2.44 2023[147]
KMT-2019-BLG-0335Lb 21 1.64 2023[158]
KMT-2019-BLG-0298Lb 1.81 5.67 2023[147]
KMT-2019-BLG-0297Lb 19 0.960 2023[158]
KMT-2018-BLG-0885Lb 29 1.07 2023[158]
KMT-2017-BLG-1194Lb 0.0111 1.78 2023[148]
KMT-2017-BLG-1003Lb 0.01633 1.38 2023[148]
KMT-2017-BLG-0428Lb 0.0176 1.81 2023[148]
KMT-2016-BLG-1105Lb 0.00730 2.44 2023[148]
K2-2016-BLG-0005Lb 1.10 4.16 4700 2023[159]
OGLE-2017-BLG-1275Lb 5.90 2.09 2024[160]
OGLE-2017-BLG-1237Lb 3.80 2.53 2024[160]
OGLE-2017-BLG-0640Lb 1.62 1.14 2024[160]

Candidate rogue planets

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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[161]
OGLE-2016-BLG-1540L ~35 M🜨 2017[162]
OGLE-2012-BLG-1323L ~2.3 M🜨 2018[163]
OGLE-2017-BLG-0560L ~1.9 MJ 2018[163]
OGLE-2019-BLG-0551L ~7.7 M🜨 2020[164]
KMT-2019-BLG-2073L ~59 M🜨 2020[165]
OGLE-2016-BLG-1928L ~0.3 M🜨 2020[166]
KMT-2017-BLG-2820L ~8.2 M🜨 2020[167]

Unconfirmed detections

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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.[168]

See also

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Notes

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  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

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  146. ^ Chung, Sun-Ju; Udalski, Andrzej; Yee, Jennifer C.; Gould, Andrew; Albrow, Michael D.; Jung, Youn Kil; Hwang, Kyu-Ha; Han, Cheongho; Ryu, Yoon-Hyun; Shin, In-Gu; Shvartzvald, Yossi; Yang, Hongjing; Zang, Weicheng; Cha, Sang-Mok; Kim, Dong-Jin (2023-12-01). "OGLE-2019-BLG-1180Lb: Discovery of a Wide-orbit Jupiter-mass Planet around a Late-type Star". The Astronomical Journal. 166 (6): 253. arXiv:2312.01278. Bibcode:2023AJ....166..253C. doi:10.3847/1538-3881/ad0723. ISSN 0004-6256.
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  148. ^ a b c d e f g Zang, Weicheng; Jung, Youn Kil; Yang, Hongjing; Zhang, Xiangyu; Udalski, Andrzej; Yee, Jennifer C.; Gould, Andrew; Mao, Shude; Albrow, Michael D.; Chung, Sun-Ju; Han, Cheongho; Hwang, Kyu-Ha; Ryu, Yoon-Hyun; Shin, In-Gu; Shvartzvald, Yossi (2023-03-01). "Systematic KMTNet Planetary Anomaly Search. VII. Complete Sample of q < 10-4 Planets from the First 4 yr Survey". The Astronomical Journal. 165 (3): 103. arXiv:2210.12344. Bibcode:2023AJ....165..103Z. doi:10.3847/1538-3881/acb34b. ISSN 0004-6256.
  149. ^ Han, Cheongho; Gould, Andrew; Jung, Youn Kil; Bond, Ian A.; Zang, Weicheng; Chung, Sun-Ju; Albrow, Michael D.; Hwang, Kyu-Ha; Ryu, Yoon-Hyun; Shin, In-Gu; Shvartzvald, Yossi; Yang, Hongjing; Yee, Jennifer C.; Cha, Sang-Mok; Kim, Doeon (2023-06-01). "MOA-2022-BLG-249Lb: Nearby microlensing super-Earth planet detected from high-cadence surveys". Astronomy and Astrophysics. 674: A89. arXiv:2304.02815. Bibcode:2023A&A...674A..89H. doi:10.1051/0004-6361/202346166. ISSN 0004-6361.
  150. ^ Olmschenk, Greg; Bennett, David P.; Bond, Ian A.; Zang, Weicheng; Jung, Youn Kil; Yee, Jennifer C.; Bachelet, Etienne; Abe, Fumio; Barry, Richard K.; Bhattacharya, Aparna; Fujii, Hirosane; Fukui, Akihiko; Hirao, Yuki; Silva, Stela Ishitani; Itow, Yoshitaka (2023-04-01). "MOA-2020-BLG-208Lb: Cool Sub-Saturn-mass Planet within Predicted Desert". The Astronomical Journal. 165 (4): 175. arXiv:2210.02436. Bibcode:2023AJ....165..175O. doi:10.3847/1538-3881/acbcc8. ISSN 0004-6256.
  151. ^ a b Han, Cheongho; Lee, Chung-Uk; Zang, Weicheng; Jung, Youn Kil; Christie, Grant W.; Zhang, Jiyuan; Albrow, Michael D.; Chung, Sun-Ju; Gould, Andrew; Hwang, Kyu-Ha; Kim, Doeon; Ryu, Yoon-Hyun; Shin, In-Gu; Shvartzvald, Yossi; Yang, Hongjing (2023-06-01). "KMT-2021-BLG-2010Lb, KMT-2022-BLG-0371Lb, and KMT-2022-BLG-1013Lb: Three microlensing planets detected via partially covered signals". Astronomy and Astrophysics. 674: A90. arXiv:2304.03871. Bibcode:2023A&A...674A..90H. doi:10.1051/0004-6361/202346298. ISSN 0004-6361.
  152. ^ Zhang, Jiyuan; Zang, Weicheng; Jung, Youn Kil; Yang, Hongjing; Gould, Andrew; Sumi, Takahiro; Mao, Shude; Dong, Subo; Albrow, Michael D.; Chung, Sun-Ju; Han, Cheongho; Hwang, Kyu-Ha; Ryu, Yoon-Hyun; Shin, In-Gu; Shvartzvald, Yossi (2023-07-01). "KMT-2022-BLG-0440Lb: A new q < 10-4 microlensing planet with the central-resonant caustic degeneracy broken". Monthly Notices of the Royal Astronomical Society. 522 (4): 6055–6069. arXiv:2301.06779. Bibcode:2023MNRAS.522.6055Z. doi:10.1093/mnras/stad1398. ISSN 0035-8711.
  153. ^ a b c d Ryu, Yoon-Hyun; Shin, In-Gu; Yang, Hongjing; Gould, Andrew; Albrow, Michael D.; Chung, Sun-Ju; Han, Cheongho; Hwang, Kyu-Ha; Kil Jung, Youn; Shvartzvald, Yossi; Yee, Jennifer C.; Zang, Weicheng; Cha, Sang-Mok; Kim, Dong-Jin; Kim, Seung-Lee (2023-03-01). "Mass Production of 2021 KMTNet Microlensing Planets II". The Astronomical Journal. 165 (3): 83. arXiv:2207.07295. Bibcode:2023AJ....165...83R. doi:10.3847/1538-3881/acab6b. ISSN 0004-6256.
  154. ^ Han, Cheongho; Lee, Chung-Uk; Zang, Weicheng; Jung, Youn Kil; Christie, Grant W.; Zhang, Jiyuan; Albrow, Michael D.; Chung, Sun-Ju; Gould, Andrew; Hwang, Kyu-Ha; Kim, Doeon; Ryu, Yoon-Hyun; Shin, In-Gu; Shvartzvald, Yossi; Yang, Hongjing (2023-06-01). "KMT-2021-BLG-2010Lb, KMT-2022-BLG-0371Lb, and KMT-2022-BLG-1013Lb: Three microlensing planets detected via partially covered signals". Astronomy and Astrophysics. 674: A90. arXiv:2304.03871. Bibcode:2023A&A...674A..90H. doi:10.1051/0004-6361/202346298. ISSN 0004-6361.
  155. ^ Han, Cheongho; Jung, Youn Kil; Bond, Ian A.; Chung, Sun-Ju; Albrow, Michael D.; Gould, Andrew; Hwang, Kyu-Ha; Lee, Chung-Uk; Ryu, Yoon-Hyun; Shin, In-Gu; Shvartzvald, Yossi; Yang, Hongjing; Yee, Jennifer C.; Zang, Weicheng; Cha, Sang-Mok (2023-10-01). "Brown dwarf companions in binaries detected in the 2021 season high-cadence microlensing surveys". Astronomy and Astrophysics. 678: A190. arXiv:2307.04921. Bibcode:2023A&A...678A.190H. doi:10.1051/0004-6361/202347014. ISSN 0004-6361.
  156. ^ Han, Cheongho; Zang, Weicheng; Jung, Youn Kil; Bond, Ian A.; Chung, Sun-Ju; Albrow, Michael D.; Gould, Andrew; Hwang, Kyu-Ha; Ryu, Yoon-Hyun; Shin, In-Gu; Shvartzvald, Yossi; Yang, Hongjing; Yee, Jennifer C.; Cha, Sang-Mok; Kim, Doeon (2023-10-01). "KMT-2021-BLG-1547Lb: Giant microlensing planet detected through a signal deformed due to source binarity". Astronomy and Astrophysics. 678: A101. arXiv:2309.01280. Bibcode:2023A&A...678A.101H. doi:10.1051/0004-6361/202347366. ISSN 0004-6361.
  157. ^ Han, Cheongho; Jung, Youn Kil; Bond, Ian A.; Gould, Andrew; Chung, Sun-Ju; Albrow, Michael D.; Hwang, Kyu-Ha; Ryu, Yoon-Hyun; Shin, In-Gu; Shvartzvald, Yossi; Yang, Hongjing; Yee, Jennifer C.; Zang, Weicheng; Cha, Sang-Mok; Kim, Doeon (2023-07-01). "KMT-2021-BLG-1150Lb: Microlensing planet detected through a densely covered planetary-caustic signal". Astronomy and Astrophysics. 675: A36. arXiv:2305.15628. Bibcode:2023A&A...675A..36H. doi:10.1051/0004-6361/202346596. ISSN 0004-6361.
  158. ^ a b c Han, Cheongho; Kil Jung, Youn; Kim, Doeon; Gould, Andrew; Bozza, Valerio; Bond, Ian A.; Chung, Sun-Ju; Albrow, Michael D.; Hwang, Kyu-Ha; Ryu, Yoon-Hyun; Shin, In-Gu; Shvartzvald, Yossi; Yang, Hongjing; Zang, Weicheng; Cha, Sang-Mok (2023-07-01). "Probable brown dwarf companions detected in binary microlensing events during the 2018-2020 seasons of the KMTNet survey". Astronomy and Astrophysics. 675: A71. arXiv:2305.06605. Bibcode:2023A&A...675A..71H. doi:10.1051/0004-6361/202245455. ISSN 0004-6361.
  159. ^ Specht, D.; Poleski, R.; Penny, M. T.; Kerins, E.; McDonald, I.; Lee, Chung-Uk; Udalski, A.; Bond, I. A.; Shvartzvald, Y.; Zang, Weicheng; Street, R. A.; Hogg, D. W.; Gaudi, B. S.; Barclay, T.; Barentsen, G. (2023-04-01). "Kepler K2 Campaign 9 - II. First space-based discovery of an exoplanet using microlensing". Monthly Notices of the Royal Astronomical Society. 520 (4): 6350–6366. arXiv:2203.16959. Bibcode:2023MNRAS.520.6350S. doi:10.1093/mnras/stad212. ISSN 0035-8711.
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  161. ^ Freeman, M.; Philpott, L. C.; Abe, F.; Albrow, M. D.; Bennett, D. P.; Bond, I. A.; Botzler, C. S.; Bray, J. C.; Cherrie, J. M.; Christie, G. W.; Dionnet, Z.; Gould, A.; Han, C.; Heyrovsky, D.; McCormick, J. M.; Moorhouse, D. M.; Muraki, Y.; Natusch, T.; Rattenbury, N. J.; Skowron, J.; Sumi, T.; Suzuki, D.; Tan, T. -G.; Tristram, P. J.; Yock, P. C. M. (2014). "Can the masses of isolated planetary-mass gravitational lenses be measured by terrestrial parallax?". The Astrophysical Journal. 799 (2): 181. arXiv:1412.1546. Bibcode:2015ApJ...799..181F. doi:10.1088/0004-637X/799/2/181. S2CID 118415208.
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