J/AJ/170/75ivo://CDS.VizieR/J/AJ/170/75CDSChung S.-J.Hwang K.-H.Yee J.C.Gould A.Bond I.A.Yang H.,(the Leading Authors)Albrow M.D.Jung Y.K.Han C.Ryu Y.-H.,Shin I.-G.Shvartzvald Y.Zang W.Cha S.-M.Kim D.-J.Kim S.-L.,Lee C.-U.Lee D.-J.Lee Y.Park B.-G.Pogge R.W.,(the Kmtnet Collaboration)Abe F.Bennett D.P.Bhattacharya A.,Fukui A.Hamada R.Hirao Y.Ishitani Silva S.Koshimoto N.,Miyazaki S.Muraki Y.Nagai T.Nunota K.Olmschenk G.Ranc C.,Rattenbury N.J.Satoh Y.Sumi T.Suzuki D.Terry S.K.Tristram P.J.,Vandorou A.Yama H.(the Moa Collaboration)2026-05-28T08:28:15Z2026-05-28T09:19:27ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frgravitational-lensingphotometryvisible-astronomyastronomical-modelsmultiple-starsWe present the analysis of a microlensing event KMT-2022-BLG-0086 of which the overall light curve is not described by a binary-lens single-source (2L1S) model, which suggests the existence of an extra lens or an extra source. We found that the event is best explained by the binary-lens binary-source (2L2S) model, but the 2L2S model is only favored over the triple-lens single-source (3L1S) model by {Delta}{chi}^2^~9. Although the event has noticeable anomalies around the peak of the light curve, they are not enough covered to constrain the angular Einstein radius {theta}_E_, thus we only measure the minimum angular Einstein radius {theta}_E,min_. From the Bayesian analysis, it is found that that the binary lens system is a binary star with masses of (m_1_,m_2_)=(0.46^+0.35^_-0.25_M_{sun}_,0.75^+0.67^_-0.55_M_{sun}_) at a distance of D_L_=5.87^+1.21^_-1.79_kpc, while the triple lens system is a brown dwarf or a massive giant planet in a low-mass binary-star system with masses of (m_1_,m_2_,m_3_)= (0.43^+0.41^_-0.35_M_{sun}_,0.056^+0.055^_-0.047_M_{sun}_, 20.84^+20.20^_-17.04_M_{sun}_), at a distance of D_L_=4.06^+1.39^_-3.28_kpc, indicating a disk lens system. The 2L2S model yields the relative lens-source proper motion of {mu}_rel_>=4.6mas/yr that is consistent with the Bayesian result, whereas the 3L1S model yields {mu}_rel_>=18.9mas/yr, which is more than three times larger than that of a typical disk object of ~6mas/yr and thus is not consistent with the Bayesian result. This suggests that the event is likely caused by the binary-lens binary-source model.2025AJ....170...75Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/170/75CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/466/157 : Bulge Microlensing Events (Soto+, 2007)J/A+A/533/A134 : Abundances of microlensed stars in the Bulge (Bensby+, 2011)J/ApJ/778/150 : Microlensing events toward the Bulge from MOA-II (Sumi+, 2013)J/ApJ/827/139 : Microlensing opt. depth & event rates from MOA-II (Sumi+, 2016)J/A+A/617/A135 : 20 years of photometric microlensing (Mustill+, 2018)J/AcA/68/183 : Predicted Microlensing Events for 21st Century (Bramich+, 2018)J/ApJS/244/29 : Microlensing events toward the Galactic bulge (Mroz+, 2019)J/A+A/640/A83 : Mass determination using microlensing by Gaia (Klueter+, 2020)J/MNRAS/498/L6 : Gaia DR2 predictions of microlensing events (McGill+, 2020)J/AJ/161/293 : LCs of OGLE-2018-BLG-0567 and OGLE-2018-BLG-0962 (Jung+, 2021)J/AJ/163/176 : Prediction of microlensing events with Gaia EDR3 (Kluter+, 2022)J/A+A/674/A23 : Gaia DR3 Microlensing events (Wyrzykowski+, 2023)J/AJ/165/83 : KMTNet light curve for 4 microlensing planets (Ryu+, 2023)J/AJ/169/288 : LCs of microlensing events revealing planets (Han+, 2025)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/170/75https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/170/75http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/170/75https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/170/75https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/170/75http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/170/75GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/AJ/170/75/fig4List of files and plots from Figure 4 (added by CDS)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTelTelescope (1)meta.id;instr.telcharFilterFiltermeta.id;instr.filtercharModelModel (2)meta.id;stat.fitcharf_ModelSolution of the 2L2S model (wide or close)meta.code;stat.fitcharFileLink to the light curve file in MRT formatmeta.id;meta.filecharLCAssociated light curve with link to interactive plotmeta.ref.urlchar