J/AJ/170/75 LCs of KMT-2022-BLG-0086 with 2L2s & 3L1S models (Chung+, 2025) ================================================================================ KMT-2022-BLG-0086: Another binary-lens binary-source microlensing event. Chung 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) =2025AJ....170...75C ================================================================================ ADC_Keywords: Gravitational lensing; Photometry; Optical; Models; Stars, double and multiple Keywords: Gravitational microlensing Abstract: We 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. Description: The event was first discovered by the Korea Microlensing Telescope Network (KMTNet). KMTNet uses three identical 1.6m telescopes with 4deg^2^ field of view (FOV) cameras that are globally distributed at the Cerro Tololo Inter-American Observatory in Chile (KMTC), the South African Astronomical Observatory (KMTA), and the Siding Spring Observatory (KMTS) in Australia. The KMTNet observations were carried out in the I and V bands. The event lies in the KMT subprime field BLG15 with a cadence of {Gamma}=1/hr. The Microlensing Observations in Astrophysics (MOA) also independently found this event and it was designated as MOA-2022-BLG-130. MOA uses a 1.8m telescope with 2.2deg^2^ FOV at Mt. John Observatory in New Zealand. The MOA observations were carried out in the MOA-Red band R_MOA_ that corresponds to the sum of the Cousins R and I bands. Objects: ------------------------------------------------------------------- RA (2000) DE Designation(s) ------------------------------------------------------------------- 17 33 57.67 -27 06 02.5 KMT-2022-BLG-0086 = KMT-2022-BLG-0086 ------------------------------------------------------------------- File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file fig4.dat 48 12 List of files and plots from Figure 4 (added by CDS) lc/* . 12 Light curves files in MRT format -------------------------------------------------------------------------------- See also: J/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) Byte-by-byte Description of file: fig4.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 6 A6 --- Tel Telescope (1) 8 A1 --- Filter Filter 10- 13 A4 --- Model Model (2) 15- 19 A5 --- f_Model Solution of the 2L2S model (wide or close) 21- 45 A25 --- File Link to the light curve file in MRT format 47- 48 A2 --- LC Associated light curve with link to interactive plot -------------------------------------------------------------------------------- Note (1): Telescope as follows: KMTA15 = The 1.6m telescope from the Korea Microlensing Telescope Network (KMTNet) at the South African Astronomical Observatory (KMTA) KMTC15 = The 1.6m telescope from the Korea Microlensing Telescope Network (KMTNet) at the Cerro Tololo Inter-American Observatory in Chile (KMTC) KMTS15 = The 1.6m telescope from the Korea Microlensing Telescope Network (KMTNet) at the Siding Spring Observatory (KMTS) in Australia MOA = The 1.8m telescope from the Microlensing Observations in Astrophysics (MOA) at Mt. John Observatory in New Zealand Note (2): Models as follows: 2L2S = Binary-lens binary-source (2L2S) model (See Section 3.2) 3L1S = Triple-lens single-source (3L1S) model (See Section 3.3) -------------------------------------------------------------------------------- History: From electronic version of the journal License: CC-BY-4.0 ================================================================================ (End) Prepared by [AAS], Robin Leichtnam [CDS] 26-May-2026