Mass Production of 2021 KMTNet Microlensing Planets. I

Ryu, Yoon-Hyun; Jung, Youn Kil; Yang, Hongjing; Gould, Andrew; Albrow, M. D.; Chung, Sun-Ju; Han, Cheongho; Hwang, Kyu-Ha; Shin, In-Gu; Shvartzvald, Yossi; Yee, Jennifer C.; Zang, Weicheng; Cha, Sang-Mok; Kim, Dong-Jin; Kim, S.-L.; Lee, Chung-Uk; Lee, Dong-Joo; Lee, Yongseok; Park, Byeong-Gon; Pogge, Richard W.

doi:10.3847/1538-3881/ac8d6c

“…This paper is the third in our series that aims to publish all by-eye planet detections from the 2021 Korea Microlensing Telescope Network (KMTNet; Kim et al 2016) observing season. Previously, in Ryu et al (2022a) and Ryu et al (2022b), we published eight planet detections; 10 other planets from the 2021 season have been published in other work (Han et al 2022a(Han et al , 2022b(Han et al , 2022c(Han et al , 2022dYang et al 2022).…”

Section: Introductionmentioning

confidence: 86%

“…Here we present the analysis of three additional planetary events: KMT-2021-BLG-0119, KMT-2021-BLG-0192, and KMT-2021-BLG-2294 The three planetary events were identified by IGS (the first author of this paper) using the traditional "by-eye" selection (described in Ryu et al 2022a). However, because IGS uses a variation on a method that was previously described, we document that here.…”

Section: Introductionmentioning

confidence: 99%

Mass Production of 2021 KMTNet Microlensing Planets. III. Analysis of Three Giant Planets

Shin

¹

,

Yee

²

,

Gould

³

et al. 2022

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We present the analysis of three more planets from the KMTNet 2021 microlensing season. KMT-2021-BLG-0119Lb is a ∼6M Jup planet orbiting an early M dwarf or a K dwarf, KMT-2021-BLG-0192Lb is a ∼2M Nep planet orbiting an M dwarf, and KMT-2021-BLG-2294Lb is a ∼1.25M Nep planet orbiting a very-low-mass M dwarf or a brown dwarf. These by-eye planet detections provide an important comparison sample to the sample selected with the AnomalyFinder algorithm, and in particular, KMT-2021-BLG-2294 is a case of a planet detected by eye but not by algorithm. KMT-2021-BLG-2294Lb is part of a population of microlensing planets around very-low-mass host stars that spans the full range of planet masses, in contrast to the planet population at ≲0.1 au, which shows a strong preference for small planets.

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“…We often make use of the heuristic analysis introduced by Hwang et al (2022) and modified by Ryu et al (2022) based on further investigation in Gould et al (2022). If a brief anomaly at t anom is treated as due to the source crossing the planet-host axis, then one can estimate two relevant parameters 2 , and τ anom = (t anom − t 0 )/t E .…”

Section: Preamblementioning

confidence: 99%

“…To test this prediction in individual cases, we can compare the purely empirical quantity † º + -s s s with the prediction from Equation (2), which we always label with a subscript, i.e., either † + s or † -s . This formalism can also be used to find "missing solutions" that have been missed in the grid search, as was done, e.g., for the case of KMT-2021-BLG-1391 (Ryu et al 2022).…”

Section: Preamblementioning

confidence: 99%

“…The grid search returns two solutions, whose refinements are given in Table 4 and whose geometries are shown in Figure 3. Note that both geometries have the source crossing the neck of a resonant caustic, which does not appear to be directly related to either of the degeneracies (inner-outer of Gaudi & Gould 1997; or close-wide of Griest & Safizadeh 1998) that were predicted in advance and that were unified in Equation (2) by Ryu et al (2022) following the conjecture of Yee et al (2021). Subsequently, Zhang & Gaudi (2022) investigated the origins of unification at the level of the lens equation.…”

Section: Kmt-2018-blg-0247mentioning

confidence: 99%

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Systematic KMTNet Planetary Anomaly Search. VI. Complete Sample of 2018 Sub-prime-field Planets

Jung

¹

,

Zang

²

,

Han

³

et al. 2022

AJ

Self Cite

20

0

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We complete the analysis of all 2018 sub-prime-field microlensing planets identified by the KMTNet AnomalyFinder. Among the 9 previously unpublished events with clear planetary solutions, 6 are clearly planetary (OGLE-2018-BLG-0298, KMT-2018-BLG-0087, KMT-2018-BLG-0247, KMT-2018-BLG-0030, OGLE-2018-BLG-1119, and KMT-2018-BLG-2602), while the remaining 3 are ambiguous in nature. The above ordering of these events is made to facilitate grouping of their Bayesian estimates: the first two are lower-mass gas giants while the last four are Jovian-class planets; the first three most likely lie in the bulge, the last in the disk, and the remaining two are equally likely to be in either population. More specifically, these six planets have host masses M host = ( 0.69 − 0.30 + 0.34 , 0.10 − 0.05 + 0.14 , 0.29 − 0.14 + 0.28 , 0.51 − 0.31 + 0.43 , 0.48 − 0.28 + 0.35 , 0.66 − 0.36 + 0.42 ) M ⊙ , planet masses M planet = ( 0.14 − 0.06 + 0.07 , 0.23 − 0.12 + 0.32 , 2.11 − 1.04 + 2.09 , 1.45 − 0.88 + 1.23 , 0.91 − 0.52 + 0.66 , 1.15 − 0.63 + 0.73 ) M Jup , and distances D L = ( 6.54 − 1.23 + 0.95 , 7.02 − 1.15 + 1.03 , 6.76 − 1.24 + 0.99 , 6.48 − 1.96 + 1.28 , 5.76 − 2.48 + 1.43 , 4.31 − 1.84 + 1.97 ) kpc . In addition, there are 8 previously published sub-prime-field planets that were selected by the AnomalyFinder algorithm. Together with a companion paper on 2018 prime-field planets, this work lays the basis for comprehensive statistical studies. We carry out two such studies, one on caustic topologies and the other on the role of Gaia data. From the first, as expected, half (17/33) of the 2018 planets likely to enter the mass-ratio analysis have non-caustic-crossing anomalies. However, only 1 of the 5 noncaustic anomalies with planet-host mass ratio q < 10−3 was discovered by eye (compared to 7 of the 12 with q > 10−3), showing the importance of the semiautomated AnomalyFinder search. From the second, we find that Gaia has played a major role in the interpretation of 16% of the sample and a supplementary role in 6%.

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MOA-2022-BLG-249Lb: Nearby microlensing super-Earth planet detected from high-cadence surveys

Han¹,

Gould²,

Jung³

et al. 2023

A&A

4

0

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Aims. We investigate the data collected by the high-cadence microlensing surveys during the 2022 season in search of planetary signals appearing in the light curves of microlensing events. From this search, we find that the lensing event MOA-2022-BLG-249 exhibits a brief positive anomaly that lasted for about one day, with a maximum deviation of ~0.2 mag from a single-source, single-lens model. Methods. We analyzed the light curve under the two interpretations of the anomaly: one originated by a low-mass companion to the lens (planetary model) and the other originated by a faint companion to the source (binary-source model). Results. We find that the anomaly is better explained by the planetary model than the binary-source model. We identified two solutions rooted in the inner-outer degeneracy and for both of them, the estimated planet-to-host mass ratio, q ~ 8 × 10−5, is very small. With the constraints provided by the microlens parallax and the lower limit on the Einstein radius, as well as the blend-flux constraint, we find that the lens is a planetary system, in which a super-Earth planet, with a mass of (4.83 ± 1.44) Μ⊕, orbits a low-mass host star, with a mass of (0.18 ± 0.05) M⊙, lying in the Galactic disk at a distance of (2.00 ± 0.42) kpc. The planet detection demonstrates the elevated microlensing sensitivity of the current high-cadence lensing surveys to low-mass planets.

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Mass Production of 2021 KMTNet Microlensing Planets. I

Cited by 17 publications

References 49 publications

Mass Production of 2021 KMTNet Microlensing Planets. III. Analysis of Three Giant Planets

Mass Production of 2021 KMTNet Microlensing Planets. III. Analysis of Three Giant Planets

Systematic KMTNet Planetary Anomaly Search. VI. Complete Sample of 2018 Sub-prime-field Planets

MOA-2022-BLG-249Lb: Nearby microlensing super-Earth planet detected from high-cadence surveys

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