KMT-2018-BLG-1743: planetary microlensing event occurring on two source stars

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

doi:10.1051/0004-6361/202140923

Cited by 11 publications

(10 citation statements)

References 53 publications

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“…It is found that the 2L2S models yield better fits than the 3L1S models by ∆χ 2 = [10.8 − 12.5]. If the 2L2S interpretation is correct, KMT-2021-BLG-0240 is the sixth lensing event for which both the lens and source are binaries, following MOA-2010-BLG-117 (Bennett et al 2018), OGLE-2016-BLG-1003 (Jung et al 2017), KMT-2018-BLG-1743(Han et al 2021a, KMT-2019-BLG-0797 (Han et al 2021b), and KMT-2021-BLG-1898(Han et al 2022b. Except for OGLE-2016-BLG-1003, the lenses of the other five events, including the event analyzed in this work, are planetary systems, indicating that planetary signals detectable through the high-magnification channel are prone to be affected by close companions to source stars.…”

Section: Binary-lens Binary-source (2l2s) Interpretationmentioning

confidence: 99%

“…There are four events with such deformations, including OGLE-2007-BLG-349 (Bennett et al 2016), OGLE-2016-BLG-0613 (Han et al 2017), OGLE-2018-BLG-1700 (Han et al 2020b), and KMT-2020-BLG-0414 (Zang et al 2021a). Finally, the central-caustic signal can also be deformed by the close companion to the source, as illustrated by three lensing events of MOA-2010-BLG-117 (Bennett et al 2018), KMT-2018-BLG-1743(Han et al 2021a, KMT-2021-BLG-1898(Han et al 2022b.…”

Section: Introductionmentioning

confidence: 99%

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KMT-2021-BLG-0240: Microlensing event with a deformed planetary signal

Han,

Kim,

Yang

et al. 2022

Preprint

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Aims. The light curve of the microlensing event KMT-2021-BLG-0240 exhibits a short-lasting anomaly with complex features near the peak at the 0.1 mag level from a single-lens single-source model. We conducted modeling of the lensing light curve under various interpretations to reveal the nature of the anomaly. Methods. It is found that the anomaly cannot be explained with the usual model based on a binary-lens (2L1S) or a binary-source (1L2S) interpretation. However, a 2L1S model with a planet companion can describe part of the anomaly, suggesting that the anomaly may be deformed by a tertiary lens component or a close companion to the source. From the additional modeling, we find that all the features of the anomaly can be explained with either a triple-lens (3L1S) model or a binary-lens binary-source (2L2S) model obtained under the 3L1S interpretation. However, it is difficult to validate the 2L2S model because the light curve does not exhibit signatures induced by the source orbital motion and the ellipsoidal variations expected by the close separation between the source stars according to the model. We, therefore, conclude that the two interpretations cannot be distinguished with the available data, and either can be correct.Results. According to the 3L1S solution, the lens is a planetary system with two sub-Jovian-mass planets in which the planets have masses of 0.32-0.47 M J and 0.44-0.93 M J , and they orbit an M dwarf host. According to the 2L2S solution, on the other hand, the lens is a single planet system with a mass of ∼ 0.21 M J orbiting a late K-dwarf host, and the source is a binary composed of a primary of a subgiant or a turnoff star and a secondary of a late G dwarf. The distance to the planetary system varies depending on the solution: ∼ 7.0 kpc according to the 3L1S solution and ∼ 6.6 kpc according to the 2L2S solution.

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Section: Binary-lens Binary-source (2l2s) Interpretationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

KMT-2021-BLG-0240: Microlensing event with a deformed planetary signal

Han,

Kim,

Yang

et al. 2022

Preprint

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“…We made an additional check with a 2L2S model, in which both the lens and source are binaries; such a system is exemplified by MOA-2010-BLG-117 (Bennett et al 2018), OGLE-2016-BLG-1003 (Jung et al 2017), KMT-2019-BLG-0797 (Han et al 2021b), and KMT-2018-BLG-1743 (Han et al 2021a). The model curve and residual from the 2L2S solution are presented in Fig.…”

Section: L1s 1l2s and 2l2s Modelsmentioning

confidence: 99%

OGLE-2019-BLG-0468Lb,c: Two microlensing giant planets around a G-type star

Han

Udalski

Lee

et al. 2022

A&A

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Aims. With the aim of interpreting anomalous lensing events with no suggested models, we conducted a project of reinvestigating microlensing data collected in and before the 2019 season. In this work, we report a multi-planet system, OGLE-2019-BLG-0468L, that was found as a result of this project. Methods. The light curve of the lensing event OGLE-2019-BLG-0468, which consists of three distinctive anomaly features, could not be explained by the usual binary-lens or binary-source interpretations. We find a solution that explains all anomaly features with a triple-lens interpretation, in which the lens is composed of two planets and their host, making the lens the fourth multi-planet system securely found by microlensing. Results. The two planets have masses of ~3.4 MJ and ~10.2 MJ, and they are orbiting around a G-type star with a mass of ~0.9 M⊙ and a distance of ~4.4 kpc. The host of the planets is most likely responsible for the light of the baseline object, although the possibility of the host being a companion to the baseline object cannot be ruled out.

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“…This additional lens component can be a second planet, as in the cases of OGLE-2006-BLG-109 (Gaudi et al 2008Bennett et al 2010), OGLE-2012-BLG-0026 (Han et al 2013), and OGLE-2018-BLG-1011 (Han et al 2019), or a binary companion to the host, as in the cases of OGLE-2007-BLG-349 (Bennett et al 2016, KMT-2020-BLG-0414 (Zang et al 2021), OGLE-2016-BLG-0613 (Han et al 2017), and OGLE-2018-BLG-1700 (Han et al 2020). Another major cause of a deformation is the binarity of the source, as illustrated by the lensing events MOA-2010-BLG-117 (Bennett et al 2018) and KMT-2018-BLG-1743 (Han et al 2021a). For the lensing event KMT-2019-BLG-1715, an even more complicated model with three lens masses (binary stars and a planet) and two source stars is needed to explain the deformed anomalies in the lensing light curve (Han et al 2021c).…”

Section: Introductionmentioning

confidence: 99%

KMT-2021-BLG-1898: Planetary microlensing event involved with binary source stars

Han¹,

Gould²,

Kim³

et al. 2022

A&A

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Aims. The light curve of the microlensing event KMT-2021-BLG-1898 exhibits a short-term central anomaly with double-bump features that cannot be explained by the usual binary-lens or binary-source interpretations. With the aim of interpreting the anomaly, we analyze the lensing light curve under various sophisticated models. Methods. We find that the anomaly is explained by a model, in which both the lens and source are binaries (2L2S model). For this interpretation, the lens is a planetary system with a planet/host mass ratio of q ~ 1.5 × 10−3, and the source is a binary composed of a turn off or a subgiant star and a mid K dwarf. The double-bump feature of the anomaly can also be depicted by a triple-lens model (3L1S model), in which the lens is a planetary system containing two planets. Among the two interpretations, the 2L2S model is favored over the 3L1S model not only because it yields a better fit to the data, by ∆χ2 = [14.3−18.5], but also the Einstein radii derived independently from the two stars of the binary source result in consistent values. According to the 2L2S interpretation, KMT-2021-BLG-1898 is the third planetary lensing event occurring on a binary stellar system, following MOA-2010-BLG-117 and KMT-2018-BLG-1743. Results. Under the 2L2S interpretation, we identify two solutions resulting from the close-wide degeneracy in determining the planet-host separation. From a Bayesian analysis, we estimate that the planet has a mass of ~0.7−0.8 MJ, and it orbits an early M dwarf host with a mass of ~0.5 M⊙. The projected planet-host separation is ~1.9 AU and ~3.0 AU according to the close and wide solutions, respectively.

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KMT-2018-BLG-1743: planetary microlensing event occurring on two source stars

Cited by 11 publications

References 53 publications

KMT-2021-BLG-0240: Microlensing event with a deformed planetary signal

KMT-2021-BLG-0240: Microlensing event with a deformed planetary signal

OGLE-2019-BLG-0468Lb,c: Two microlensing giant planets around a G-type star

KMT-2021-BLG-1898: Planetary microlensing event involved with binary source stars

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