Kmt-2022-Blg-0440lb: A New q < 10−4 Microlensing Planet With the Central-Resonant Caustic Degeneracy Broken

We present the observations and analysis of a high-magnification microlensing planetary event, KMT-2022-BLG-0440, for which the weak and short-lived planetary signal was covered by both the KMTNet survey and follow-up observations. The binary-lens models with a central caustic provide the best fits,...

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Published inMonthly notices of the Royal Astronomical Society Vol. 522; no. 4; pp. 6055 - 6069
Main Authors Zhang, Jiyuan, Zang, Weicheng, Jung, Youn Kil, Yang, Hongjing, Gould, Andrew, Sumi, Takahiro, Mao, Shude, Dong, Subo, Albrow, Michael D, Chung, Sun-Ju, Han, Cheongho, Hwang, Kyu-Ha, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Yee, Jennifer C, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Chung-Uk, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W, Qian, Qiyue, Liu, Zhuokai, Maoz, Dan, Penny, Matthew T, Zhu, Wei, Abe, Fumio, Barry, Richard, Bennett, David P, Bhattacharya, Aparna, Bond, Ian A, Silva, Stela Ishitani, Koshimoto, Naoki, Olmschenk, Greg, Vandorou, Aikaterini
Format Journal Article
LanguageEnglish
Published Goddard Space Flight Center Oxford University Press (United Kingdom) 11.05.2023
Oxford University Press
Subjects
Online AccessGet full text
ISSN0035-8711
1365-2966
DOI10.1093/mnras/stad1398

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Abstract We present the observations and analysis of a high-magnification microlensing planetary event, KMT-2022-BLG-0440, for which the weak and short-lived planetary signal was covered by both the KMTNet survey and follow-up observations. The binary-lens models with a central caustic provide the best fits, with a planet/host mass ratio, q = 0.75–1.00 ×10−4 at 1 σ. The binary-lens models with a resonant caustic and a brown-dwarf mass ratio are both excluded by ∆χ2 > 70. The binary-source 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 Neptune-mass, and the projected planet-host separation is 1.9+0.6−0.7 or 4.6+1.4−1.7 au, subject to the close/wide de generac y. This is the third q < 10−4 planet from a high-magnification planetary signal ( A ≳ 65). Together with another such planet, KMT-2021-BLG-0171Lb, the ongoing follow-up program for the KMTNet high-magnification events has demonstrated its ability to detect high-magnification planetary signals for q < 10−4 planets, which are challenging for the current microlensing surveys.
AbstractList We present the observations and analysis of a high-magnification microlensing planetary event, KMT-2022-BLG-0440, for which the weak and short-lived planetary signal was covered by both the KMTNet survey and follow-up observations. The binary-lens models with a central caustic provide the best fits, with a planet/host mass ratio, q = 0.75–1.00 ×10−4 at 1 σ. The binary-lens models with a resonant caustic and a brown-dwarf mass ratio are both excluded by ∆χ2 > 70. The binary-source 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 Neptune-mass, and the projected planet-host separation is 1.9+0.6−0.7 or 4.6+1.4−1.7 au, subject to the close/wide de generac y. This is the third q < 10−4 planet from a high-magnification planetary signal ( A ≳ 65). Together with another such planet, KMT-2021-BLG-0171Lb, the ongoing follow-up program for the KMTNet high-magnification events has demonstrated its ability to detect high-magnification planetary signals for q < 10−4 planets, which are challenging for the current microlensing surveys.
We present the observations and analysis of a high-magnification microlensing planetary event, KMT-2022-BLG-0440, for which the weak and short-lived planetary signal was covered by both the KMTNet survey and follow-up observations. The binary-lens 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 binary-lens models with a resonant caustic and a brown-dwarf mass ratio are both excluded by Δχ2 > 70. The binary-source 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 Neptune-mass, and the projected planet-host 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 high-magnification planetary signal (A ≳ 65). Together with another such planet, KMT-2021-BLG-0171Lb, the ongoing follow-up program for the KMTNet high-magnification events has demonstrated its ability to detect high-magnification planetary signals for q < 10−4 planets, which are challenging for the current microlensing surveys.
ABSTRACT We present the observations and analysis of a high-magnification microlensing planetary event, KMT-2022-BLG-0440, for which the weak and short-lived planetary signal was covered by both the KMTNet survey and follow-up observations. The binary-lens 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 binary-lens models with a resonant caustic and a brown-dwarf mass ratio are both excluded by Δχ2 > 70. The binary-source 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 Neptune-mass, and the projected planet-host 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 high-magnification planetary signal (A ≳ 65). Together with another such planet, KMT-2021-BLG-0171Lb, the ongoing follow-up program for the KMTNet high-magnification events has demonstrated its ability to detect high-magnification planetary signals for q < 10−4 planets, which are challenging for the current microlensing surveys.
Audience PUBLIC
Author Mao, Shude
Pogge, Richard W
Silva, Stela Ishitani
Cha, Sang-Mok
Yee, Jennifer C
Kim, Dong-Jin
Jung, Youn Kil
Albrow, Michael D
Zhang, Jiyuan
Zhu, Wei
Kim, Seung-Lee
Sumi, Takahiro
Shvartzvald, Yossi
Ryu, Yoon-Hyun
Gould, Andrew
Maoz, Dan
Lee, Dong-Joo
Barry, Richard
Abe, Fumio
Olmschenk, Greg
Vandorou, Aikaterini
Koshimoto, Naoki
Zang, Weicheng
Han, Cheongho
Bennett, David P
Lee, Chung-Uk
Qian, Qiyue
Lee, Yongseok
Penny, Matthew T
Bond, Ian A
Yang, Hongjing
Liu, Zhuokai
Dong, Subo
Park, Byeong-Gon
Chung, Sun-Ju
Kim, Hyoun-Woo
Shin, In-Gu
Hwang, Kyu-Ha
Bhattacharya, Aparna
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Issue 4
Keywords Gravitational Lensing: Micro
Planets And Satellites: Detection
gravitational lensing: micro
planets and satellites: detection
Language English
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Notes GSFC
Goddard Space Flight Center
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Snippet We present the observations and analysis of a high-magnification microlensing planetary event, KMT-2022-BLG-0440, for which the weak and short-lived planetary...
ABSTRACT We present the observations and analysis of a high-magnification microlensing planetary event, KMT-2022-BLG-0440, for which the weak and short-lived...
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SubjectTerms Astronomy
Title Kmt-2022-Blg-0440lb: A New q < 10−4 Microlensing Planet With the Central-Resonant Caustic Degeneracy Broken
URI https://ntrs.nasa.gov/citations/20240013688
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