The gravitational microlensing technique is most sensitive to planets in a Jupiterlike orbit and has detected more than 200 planets. However, only a few wideorbit (
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Abstract s > 2) microlensing planets have been discovered, wheres is the planettohost separation normalized to the angular Einstein ring radius,θ _{E}. Here, we present the discovery and analysis of a strong candidate wideorbit microlensing planet in the event OGLE2017BLG0448. The whole light curve exhibits longterm residuals to the static binarylens singlesource model, so we investigate the residuals by adding the microlensing parallax, microlensing xallarap, an additional lens, or an additional source. For the first time, we observe a complex degeneracy between all four effects. The wideorbit models withs ∼ 2.5 and a planettohost mass ratio ofq ∼ 10^{−4}are significantly preferred, but we cannot rule out the close models withs ∼ 0.35 andq ∼ 10^{−3}. A Bayesian analysis based on a Galactic model indicates that, despite the complicated degeneracy, the surviving wideorbit models all contain a superEarthmass to Neptunemass planet at a projected planethost separation of ∼6 au and the surviving closeorbit models all consist of a Jovianmass planet at ∼1 au. The host star is probably an M or K dwarf. We discuss the implications of this dimensiondegeneracy disaster on microlensing lightcurve analysis and its potential impact on statistical studies. 
Abstract Following Shin et al. (2023b), which is a part of the “Systematic KMTNet Planetary Anomaly Search” series (i.e., a search for planets in the 2016 KMTNet prime fields), we conduct a systematic search of the 2016 KMTNet subprime fields using a semimachinebased algorithm to identify hidden anomalous events missed by the conventional byeye search. We find four new planets and seven planet candidates that were buried in the KMTNet archive. The new planets are OGLE2016BLG1598Lb, OGLE2016BLG1800Lb, MOA2016BLG526Lb, and KMT2016BLG2321Lb, which show typical properties of microlensing planets, i.e., giant planets orbit Mdwarf host stars beyond their snow lines. For the planet candidates, we find planet/binary or 2L1S/1L2S degeneracies, which are an obstacle to firmly claiming planet detections. By combining the results of Shin et al. (2023b) and this work, we find a total of nine hidden planets, which is about half the number of planets discovered by eye in 2016. With this work, we have met the goal of the systematic search series for 2016, which is to build a complete microlensing planet sample. We also show that our systematic searches significantly contribute to completing the planet sample, especially for planet/host mass ratios smaller than 10^{−3}, which were incomplete in previous byeye searches of the KMTNet archive.

Aims. We systematically inspected the microlensing data acquired by the KMTNet survey during the previous seasons in order to find anomalous lensing events for which the anomalies in the lensing light curves cannot be explained by the usual binarylens or binarysource interpretations. Methods. From the inspection, we find that interpreting the three lensing events OGLE2018BLG0584, KMT2018BLG2119, and KMT2021BLG1122 requires fourbody (lens+source) models, in which either both the lens and source are binaries (2L2S event) or the lens is a triple system (3L1S event). Following the analyses of the 2L2S events presented in our previous work, here we present the 3L1S analysis of the KMT2021BLG1122. Results. It is found that the lens of the event KMT2021BLG1122 is composed of three masses, in which the projected separations (normalized to the angular Einstein radius) and mass ratios between the lens companions and the primary are ( s 2 , q 2 )∼(1.4, 0.53) and ( s 3 , q 3 )∼(1.6, 0.24). By conducting a Bayesian analysis, we estimate that the masses of the individual lens components are ( M 1 , M 2 , M 3 )∼(0.47 M ⊙ , 0.24 M ⊙ , 0.11 M ⊙ ). The companions are separated in projection from the primary by ( a ⊥, 2 , a ⊥, 3 )∼(3.5, 4.0) AU. The lens of KMT2018BLG2119 is the first triple stellar system detected via microlensing.more » « less

ABSTRACT In this work, we update and develop algorithms for KMTNet tenderlove care (TLC) photometry in order to create a new, mostly automated, TLC pipeline. We then start a project to systematically apply the new TLC pipeline to the historic KMTNet microlensing events, and search for buried planetary signals. We report the discovery of such a planet candidate in the microlensing event MOA2019BLG421/KMT2019BLG2991. The anomalous signal can be explained by either a planet around the lens star or the orbital motion of the source star. For the planetary interpretation, despite many degenerate solutions, the planet is most likely to be a Jovian planet orbiting an M or K dwarf, which is a typical microlensing planet. The discovery proves that the project can indeed increase the sensitivity of historic events and find previously undiscovered signals.

Abstract We present the analysis of seven microlensing planetary events with planet/host mass ratios q < 10 −4 : KMT2017BLG1194, KMT2017BLG0428, KMT2019BLG1806, KMT2017BLG1003, KMT2019BLG1367, OGLE2017BLG1806, and KMT2016BLG1105. They were identified by applying the Korea Microlensing Telescope Network (KMTNet) AnomalyFinder algorithm to 2016–2019 KMTNet events. A Bayesian analysis indicates that all the lens systems consist of a cold superEarth orbiting an M or K dwarf. Together with 17 previously published and three that will be published elsewhere, AnomalyFinder has found a total of 27 planets that have solutions with q < 10 −4 from 2016–2019 KMTNet events, which lays the foundation for the first statistical analysis of the planetary massratio function based on KMTNet data. By reviewing the 27 planets, we find that the missing planetary caustics problem in the KMTNet planetary sample has been solved by AnomalyFinder. We also find a desert of highmagnification planetary signals ( A ≳ 65), and a followup project for KMTNet highmagnification events could detect at least two more q < 10 −4 planets per year and form an independent statistical sample.more » « less

Aims. We conducted a systematic investigation of the microlensing data collected during the previous observation seasons for the purpose of reanalyzing anomalous lensing events with no suggested plausible models. Methods. We found that two anomalous lensing events, OGLE2018BLG0584 and KMT2018BLG2119, cannot be explained with the usual models based on either a binarylens singlesource (2L1S) or a singlelens binarysource (1L2S) interpretation. We tested the feasibility of explaining the light curves of the events with more sophisticated models by adding either an extra lens (3L1S model) or a source (2L2S model) component to the 2L1S lens system configuration. Results. We find that a 2L2S interpretation explains the light curves of both events well and that for each event there are a pair of solutions resulting from the close and wide degeneracy. For the event OGLE2018BLG0584, the source is a binary composed of two Ktype stars and the lens is a binary composed of two M dwarfs. For KMT2018BLG2119, the source is a binary composed of two dwarfs of G and K spectral types and the lens is a binary composed of a lowmass M dwarf and a brown dwarf.more » « less

ABSTRACT We present the observations and analysis of a highmagnification microlensing planetary event, KMT2022BLG0440, for which the weak and shortlived planetary signal was covered by both the KMTNet survey and followup observations. The binarylens models with a central caustic provide the best fits, with a planet/host mass ratio, q = 0.75–1.00 × 10−4 at 1σ. The binarylens models with a resonant caustic and a browndwarf mass ratio are both excluded by Δχ2 > 70. The binarysource model can fit the anomaly well but is rejected by the ‘colour argument’ on the second source. From Bayesian analyses, it is estimated that the host star is likely a K or M dwarf located in the Galactic disc, the planet probably has a Neptunemass, and the projected planethost separation is $1.9^{+0.6}_{0.7}$ or $4.6^{+1.4}_{1.7}$ au, subject to the close/wide degeneracy. This is the third q < 10−4 planet from a highmagnification planetary signal (A ≳ 65). Together with another such planet, KMT2021BLG0171Lb, the ongoing followup program for the KMTNet highmagnification events has demonstrated its ability to detect highmagnification planetary signals for q < 10−4 planets, which are challenging for the current microlensing surveys.more » « less

Aims. We reexamine highmagnification microlensing events in the previous data collected by the KMTNet survey with the aim of finding planetary signals that were not noticed before. In this work, we report the planetary system KMT2018BLG1988L, which was found from this investigation. Methods. The planetary signal appears as a deviation with ≲0.2 mag from a singlelens light curve and lasted for about 6 h. The deviation exhibits a pattern of a dip surrounded by weak bumps on both sides of the dip. The analysis of the lensing light curve indicates that the signal is produced by a lowmassratio ( q ~ 4 × 10 −5 ) planetary companion located near the Einstein ring of the host star. Results. The mass of the planet, M planet = 6.8 −3.5 +4.7 M ⊕ and 5.6 −2.8 +3.8 M ⊕ for the two possible solutions, estimated from the Bayesian analysis indicates that the planet is in the regime of a superEarth. The host of the planet is a disk star with a mass of M host = 0.47 −0.25 +0.33 M ⊙ and a distance of D L = 4.2 −.14 +1.8 kpc. KMT2018BLG1988Lb is the 18th known microlensing planet with a mass below the upper limit of a superEarth. The fact that 15 out of the 18 known microlensing planets with masses ≲10 M ⊕ were detected in the 5 yr following the full operation of the KMTNet survey indicates that the KMTNet database is an important reservoir of very lowmass planets.more » « less

Abstract We report the analysis of microlensing event OGLE2017BLG1038, observed by the Optical Gravitational Lensing Experiment, Korean Microlensing Telescope Network, and Spitzer telescopes. The event is caused by a giant source star in the Galactic Bulge passing over a large resonant binarylens caustic. The availability of spacebased data allows the full set of physical parameters to be calculated. However, there exists an eightfold degeneracy in the parallax measurement. The four best solutions correspond to verylowmass binaries near ( M 1 = 170 − 50 + 40 M J and M 2 = 110 − 30 + 20 M J ), or well below ( M 1 = 22.5 − 0.4 + 0.7 M J and M 2 = 13.3 − 0.3 + 0.4 M J ) the boundary between stars and brown dwarfs. A conventional analysis, with scaled uncertainties for Spitzer data, implies a verylowmass browndwarf binary lens at a distance of 2 kpc. Compensating for systematic Spitzer errors using a Gaussian process model suggests that a higher mass Mdwarf binary at 6 kpc is equally likely. A Bayesian comparison based on a galactic model favors the largermass solutions. We demonstrate how this degeneracy can be resolved within the next 10 years through infrared adaptiveoptics imaging with a 40 m class telescope.more » « less

ABSTRACT We report the discovery and analysis of a candidate triplelens singlesource (3L1S) microlensing event, OGLE2019BLG1470. This event was first classified as a normal binarylens singlesource (2L1S) event, but a careful 2L1S modelling showed that it needs an additional lens or source to fit the observed data. It is found that the 3L1S model provides the best fit, but the binarylens binarysource (2L2S) model is only disfavoured by Δχ2 ≃ 18. All of the feasible models include a planet with planettohost massratios 10−3 ≲ q ≲ 10−2. A Bayesian analysis based on a Galactic model indicates that the planet is superJovian, and the projected hostplanet separation is about 3 au. Specifically, for the bestfitting 3L1S model, the two stars have masses of $M_1=0.57^{+0.43}_{0.32}{\rm M}_{\odot}$, and $M_2=0.18^{+0.15}_{0.10}\mathrm{M}_{\odot}$ with projected separation of $1.3^{+0.5}_{0.5}$ au, and the planetary mass is $M_3=2.2^{+1.8}_{1.3}M_{\rm {Jupiter}}$. For the 2L2S model, the masses of the host star and the planet are $0.55^{+0.44}_{0.31}\mathrm{M}_{\odot }$ and $4.6^{+3.7}_{2.6}M_{\rm {Jupiter}}$, respectively. By investigating the properties of all known microlensing planets in binary systems, we find that all planets in binary systems published by the KMTNet survey are located inside the resonant caustics range with q ≳ 2 × 10−3, indicating the incompleteness of the KMTNet sample for planets in binary systems. Thus, planets in binary systems cannot be included in the current study of the KMTNet massratio function, and a systematic search for planetary anomalies in KMTNet microlensing light curves of binary systems is needed.more » « less