Four microlensing giant planets detected through signals produced by minor-image perturbations

Cheongho Han; Ian A. Bond; Chung-Uk Lee; Andrew Gould; Michael D. Albrow; Sun-Ju Chung; Kyu-Ha Hwang; Youn Kil Jung; Yoon-Hyun Ryu; Yossi Shvartzvald; In-Gu Shin; Jennifer C. Yee; Hongjing Yang; Weicheng Zang; Sang-Mok Cha; Doeon Kim; Dong-Jin Kim; Seung-Lee Kim; Dong-Joo Lee; Yongseok Lee; Byeong-Gon Park; Richard W. Pogge; Fumio Abe; Ken Bando; Richard Barry; David P. Bennett; Aparna Bhattacharya; Hirosame Fujii; Akihiko Fukui; Ryusei Hamada; Shunya  Hamada; Naoto Hamasaki; Yuki Hirao; Stela Ishitani Silva; Yoshitaka Itow; Rintaro Kirikawa; Naoki Koshimoto; Yutaka Matsubara; Shota Miyazaki; Yasushi Muraki; Tutumi Nagai; Kansuke Nunota; Greg Olmschenk; Clément Ranc; Nicholas J. Rattenbury; Yuki Satoh; Takahiro Sumi; Daisuke Suzuki; Mio Tomoyoshi; Paul J. Tristram; Aikaterini Vandorou; Hibiki Yama; Kansuke Yamashita; Etienne Bachelet; Paolo Rota; Valerio Bozza; Paweł Zielinski; Rachel A. Street; Yiannis Tsapras; Markus Hundertmark; Joachim Wambsganss; Łukasz Wyrzykowski; Roberto Figuera Jaimes; Arnaud Cassan; Martin Dominik; Krzysztof A. Rybicki; Markus Rabus

doi:10.1051/0004-6361/202450221

Four microlensing giant planets detected through signals produced by minor-image perturbations

Cheongho Han
, Ian A. Bond
, Chung-Uk Lee^*
, Andrew Gould
, Michael D. Albrow
, Sun-Ju Chung
, Kyu-Ha Hwang
, Youn Kil Jung
, Yoon-Hyun Ryu
, Yossi Shvartzvald
, In-Gu Shin
, Jennifer C. Yee
, Hongjing Yang
, Weicheng Zang
, Sang-Mok Cha
, Doeon Kim
, Dong-Jin Kim
, Seung-Lee Kim
, Dong-Joo Lee
, Yongseok Lee

Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Ken Bando, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosame Fujii, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita, Etienne Bachelet, Paolo Rota, Valerio Bozza, Paweł Zielinski, Rachel A. Street, Yiannis Tsapras, Markus Hundertmark, Joachim Wambsganss, Łukasz Wyrzykowski, Roberto Figuera Jaimes, Arnaud Cassan, Martin Dominik, Krzysztof A. Rybicki, Markus Rabus

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

Abstract

Aims. We investigated the nature of the anomalies appearing in four microlensing events KMT-2020-BLG-0757, KMT-2022-BLG-0732, KMT-2022-BLG-1787, and KMT-2022-BLG-1852. The light curves of these events commonly exhibit initial bumps followed by subsequent troughs that extend across a substantial portion of the light curves.

Methods. We performed thorough modeling of the anomalies to elucidate their characteristics. Despite their prolonged durations, which differ from the usual brief anomalies observed in typical planetary events, our analysis revealed that each anomaly in these events originated from a planetary companion located within the Einstein ring of the primary star. It was found that the initial bump arouse when the source star crossed one of the planetary caustics, while the subsequent trough feature occurred as the source traversed the region of minor image perturbations lying between the pair of planetary caustics.

Results. The estimated masses of the host and planet, their mass ratios, and the distance to the discovered planetary systems are (M_host/M⊙, M_planet/M_J, q/10⁻³, D_L/kpc) = (0.58_−0.30^+0.33, 10.71_−5.61^+6.17, 17.61 ± 2.25, 6.67_−1.30^+0.93) for KMT-2020-BLG-0757, (0.53_−0.31^+0.31, 1.12_−0.65^+0.65, 2.01 ± 0.07, 6.66_−1.84^+1.19) for KMT-2022-BLG-0732, (0.42_−0.23^+0.32, 6.64_−3.64^+4.98, 15.07 ± 0.86, 7.55_−1.30^+0.89) for KMT-2022-BLG-1787, and (0.32_−0.19^+0.34, 4.98_−2.94^+5.42, 8.74 ± 0.49, 6.27_−1.15^+0.90) for KMT-2022-BLG-1852. These parameters indicate that all the planets are giants with masses exceeding the mass of Jupiter in our solar system and the hosts are low-mass stars with masses substantially less massive than the Sun.

Original language	English
Article number	A225
Number of pages	10
Journal	Astronomy & Astrophysics
Volume	687
Early online date	16 Jul 2024
DOIs	https://doi.org/10.1051/0004-6361/202450221
Publication status	Published - Jul 2024

Keywords

Planets and satellites: detection
Gravitational lensing: micro

Access to Document

10.1051/0004-6361/202450221Licence: CC BY

Han-2024-Four-microlensing-giant-planets-A&A-687-A225-CCBY
Copyright © The Authors 2024. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. This article is published in open access under the Subscribe to Open model. Subscribe to A&A to support open access publication.
Final published version, 2.13 MBLicence: CC BY

Handle.net

Persistent link

Cite this

Han, C., Bond, I. A., Lee, C.-U., Gould, A., Albrow, M. D., Chung, S.-J., Hwang, K.-H., Jung, Y. K., Ryu, Y.-H., Shvartzvald, Y., Shin, I.-G., Yee, J. C., Yang, H., Zang, W., Cha, S.-M., Kim, D., Kim, D.-J., Kim, S.-L., Lee, D.-J., ... Rabus, M. (2024). Four microlensing giant planets detected through signals produced by minor-image perturbations. Astronomy & Astrophysics, 687, Article A225. https://doi.org/10.1051/0004-6361/202450221

@article{3a0db12af0d7471692985c584b3d9277,

title = "Four microlensing giant planets detected through signals produced by minor-image perturbations",

abstract = "Aims. We investigated the nature of the anomalies appearing in four microlensing events KMT-2020-BLG-0757, KMT-2022-BLG-0732, KMT-2022-BLG-1787, and KMT-2022-BLG-1852. The light curves of these events commonly exhibit initial bumps followed by subsequent troughs that extend across a substantial portion of the light curves. Methods. We performed thorough modeling of the anomalies to elucidate their characteristics. Despite their prolonged durations, which differ from the usual brief anomalies observed in typical planetary events, our analysis revealed that each anomaly in these events originated from a planetary companion located within the Einstein ring of the primary star. It was found that the initial bump arouse when the source star crossed one of the planetary caustics, while the subsequent trough feature occurred as the source traversed the region of minor image perturbations lying between the pair of planetary caustics. Results. The estimated masses of the host and planet, their mass ratios, and the distance to the discovered planetary systems are (Mhost/M⊙, Mplanet/MJ, q/10−3, DL/kpc) = (0.58−0.30+0.33, 10.71−5.61+6.17, 17.61 ± 2.25, 6.67−1.30+0.93) for KMT-2020-BLG-0757, (0.53−0.31+0.31, 1.12−0.65+0.65, 2.01 ± 0.07, 6.66−1.84+1.19) for KMT-2022-BLG-0732, (0.42−0.23+0.32, 6.64−3.64+4.98, 15.07 ± 0.86, 7.55−1.30+0.89) for KMT-2022-BLG-1787, and (0.32−0.19+0.34, 4.98−2.94+5.42, 8.74 ± 0.49, 6.27−1.15+0.90) for KMT-2022-BLG-1852. These parameters indicate that all the planets are giants with masses exceeding the mass of Jupiter in our solar system and the hosts are low-mass stars with masses substantially less massive than the Sun.",

keywords = "Planets and satellites: detection, Gravitational lensing: micro",

author = "Cheongho Han and Bond, \{Ian A.\} and Chung-Uk Lee and Andrew Gould and Albrow, \{Michael D.\} and Sun-Ju Chung and Kyu-Ha Hwang and Jung, \{Youn Kil\} and Yoon-Hyun Ryu and Yossi Shvartzvald and In-Gu Shin and Yee, \{Jennifer C.\} and Hongjing Yang and Weicheng Zang and Sang-Mok Cha and Doeon Kim and Dong-Jin Kim and Seung-Lee Kim and Dong-Joo Lee and Yongseok Lee and Byeong-Gon Park and Pogge, \{Richard W.\} and Fumio Abe and Ken Bando and Richard Barry and Bennett, \{David P.\} and Aparna Bhattacharya and Hirosame Fujii and Akihiko Fukui and Ryusei Hamada and Shunya Hamada and Naoto Hamasaki and Yuki Hirao and Silva, \{Stela Ishitani\} and Yoshitaka Itow and Rintaro Kirikawa and Naoki Koshimoto and Yutaka Matsubara and Shota Miyazaki and Yasushi Muraki and Tutumi Nagai and Kansuke Nunota and Greg Olmschenk and Cl{\'e}ment Ranc and Rattenbury, \{Nicholas J.\} and Yuki Satoh and Takahiro Sumi and Daisuke Suzuki and Mio Tomoyoshi and Tristram, \{Paul J.\} and Aikaterini Vandorou and Hibiki Yama and Kansuke Yamashita and Etienne Bachelet and Paolo Rota and Valerio Bozza and Pawe{\l} Zielinski and Street, \{Rachel A.\} and Yiannis Tsapras and Markus Hundertmark and Joachim Wambsganss and {\L}ukasz Wyrzykowski and Jaimes, \{Roberto Figuera\} and Arnaud Cassan and Martin Dominik and Rybicki, \{Krzysztof A.\} and Markus Rabus",

note = "Funding: Work by C.H. was supported by the grants of National Research Foundation of Korea (2019R1A2C2085. This research was supported by the Korea Astronomy and Space Science Institute under the R\&D program (Project No. 2023-1-832-03) supervised by the Ministry of Science and ICT. The MOA project is supported by JSPS KAKENHI Grant Number JP24253004, JP26247023, JP23340064, JP15H00781, JP16H06287, JP17H02871 and JP22H00153. J.C.Y., I.G.S., and S.J.C. acknowledge support from NSF Grant No. AST-2108414. Y.S. acknowledges support from NSF Grant No. 2020740. C.R. was supported by the Research fellowship of the Alexander von Humboldt Foundation. This work was authored by employees of Caltech/IPAC under Contract No. 80GSFC21R0032 with the National Aeronautics and Space Administration. V.B. is supported by PRIN 2022 CUP D53D23002590006. R.F.J. acknowledges support for this project provided by ANID{\textquoteright}s Millennium Science Initiative through grant ICN12\_009, awarded to the Millennium Institute of Astrophysics (MAS), and by ANID{\textquoteright}s Basal project FB210003. This project has received funding from the European Union{\textquoteright}s Horizon 2020 research and innovation program under grant agreement No. 101004719 (OPTICON - RadioNet Pilot). This work is supported by the Polish MNiSW grant DIR/WK/2018/12.",

year = "2024",

month = jul,

doi = "10.1051/0004-6361/202450221",

language = "English",

volume = "687",

journal = "Astronomy \& Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Han, C, Bond, IA, Lee, C-U, Gould, A, Albrow, MD, Chung, S-J, Hwang, K-H, Jung, YK, Ryu, Y-H, Shvartzvald, Y, Shin, I-G, Yee, JC, Yang, H, Zang, W, Cha, S-M, Kim, D, Kim, D-J, Kim, S-L, Lee, D-J, Lee, Y, Park, B-G, Pogge, RW, Abe, F, Bando, K, Barry, R, Bennett, DP, Bhattacharya, A, Fujii, H, Fukui, A, Hamada, R, Hamada, S, Hamasaki, N, Hirao, Y, Silva, SI, Itow, Y, Kirikawa, R, Koshimoto, N, Matsubara, Y, Miyazaki, S, Muraki, Y, Nagai, T, Nunota, K, Olmschenk, G, Ranc, C, Rattenbury, NJ, Satoh, Y, Sumi, T, Suzuki, D, Tomoyoshi, M, Tristram, PJ, Vandorou, A, Yama, H, Yamashita, K, Bachelet, E, Rota, P, Bozza, V, Zielinski, P, Street, RA, Tsapras, Y, Hundertmark, M, Wambsganss, J, Wyrzykowski, Ł, Jaimes, RF, Cassan, A, Dominik, M, Rybicki, KA & Rabus, M 2024, 'Four microlensing giant planets detected through signals produced by minor-image perturbations', Astronomy & Astrophysics, vol. 687, A225. https://doi.org/10.1051/0004-6361/202450221

TY - JOUR

T1 - Four microlensing giant planets detected through signals produced by minor-image perturbations

AU - Han, Cheongho

AU - Bond, Ian A.

AU - Lee, Chung-Uk

AU - Gould, Andrew

AU - Albrow, Michael D.

AU - Chung, Sun-Ju

AU - Hwang, Kyu-Ha

AU - Jung, Youn Kil

AU - Ryu, Yoon-Hyun

AU - Shvartzvald, Yossi

AU - Shin, In-Gu

AU - Yee, Jennifer C.

AU - Yang, Hongjing

AU - Zang, Weicheng

AU - Cha, Sang-Mok

AU - Kim, Doeon

AU - Kim, Dong-Jin

AU - Kim, Seung-Lee

AU - Lee, Dong-Joo

AU - Lee, Yongseok

AU - Park, Byeong-Gon

AU - Pogge, Richard W.

AU - Abe, Fumio

AU - Bando, Ken

AU - Barry, Richard

AU - Bennett, David P.

AU - Bhattacharya, Aparna

AU - Fujii, Hirosame

AU - Fukui, Akihiko

AU - Hamada, Ryusei

AU - Hamada, Shunya

AU - Hamasaki, Naoto

AU - Hirao, Yuki

AU - Silva, Stela Ishitani

AU - Itow, Yoshitaka

AU - Kirikawa, Rintaro

AU - Koshimoto, Naoki

AU - Matsubara, Yutaka

AU - Miyazaki, Shota

AU - Muraki, Yasushi

AU - Nagai, Tutumi

AU - Nunota, Kansuke

AU - Olmschenk, Greg

AU - Ranc, Clément

AU - Rattenbury, Nicholas J.

AU - Satoh, Yuki

AU - Sumi, Takahiro

AU - Suzuki, Daisuke

AU - Tomoyoshi, Mio

AU - Tristram, Paul J.

AU - Vandorou, Aikaterini

AU - Yama, Hibiki

AU - Yamashita, Kansuke

AU - Bachelet, Etienne

AU - Rota, Paolo

AU - Bozza, Valerio

AU - Zielinski, Paweł

AU - Street, Rachel A.

AU - Tsapras, Yiannis

AU - Hundertmark, Markus

AU - Wambsganss, Joachim

AU - Wyrzykowski, Łukasz

AU - Jaimes, Roberto Figuera

AU - Cassan, Arnaud

AU - Dominik, Martin

AU - Rybicki, Krzysztof A.

AU - Rabus, Markus

N1 - Funding: Work by C.H. was supported by the grants of National Research Foundation of Korea (2019R1A2C2085. This research was supported by the Korea Astronomy and Space Science Institute under the R&D program (Project No. 2023-1-832-03) supervised by the Ministry of Science and ICT. The MOA project is supported by JSPS KAKENHI Grant Number JP24253004, JP26247023, JP23340064, JP15H00781, JP16H06287, JP17H02871 and JP22H00153. J.C.Y., I.G.S., and S.J.C. acknowledge support from NSF Grant No. AST-2108414. Y.S. acknowledges support from NSF Grant No. 2020740. C.R. was supported by the Research fellowship of the Alexander von Humboldt Foundation. This work was authored by employees of Caltech/IPAC under Contract No. 80GSFC21R0032 with the National Aeronautics and Space Administration. V.B. is supported by PRIN 2022 CUP D53D23002590006. R.F.J. acknowledges support for this project provided by ANID’s Millennium Science Initiative through grant ICN12_009, awarded to the Millennium Institute of Astrophysics (MAS), and by ANID’s Basal project FB210003. This project has received funding from the European Union’s Horizon 2020 research and innovation program under grant agreement No. 101004719 (OPTICON - RadioNet Pilot). This work is supported by the Polish MNiSW grant DIR/WK/2018/12.

PY - 2024/7

Y1 - 2024/7

N2 - Aims. We investigated the nature of the anomalies appearing in four microlensing events KMT-2020-BLG-0757, KMT-2022-BLG-0732, KMT-2022-BLG-1787, and KMT-2022-BLG-1852. The light curves of these events commonly exhibit initial bumps followed by subsequent troughs that extend across a substantial portion of the light curves. Methods. We performed thorough modeling of the anomalies to elucidate their characteristics. Despite their prolonged durations, which differ from the usual brief anomalies observed in typical planetary events, our analysis revealed that each anomaly in these events originated from a planetary companion located within the Einstein ring of the primary star. It was found that the initial bump arouse when the source star crossed one of the planetary caustics, while the subsequent trough feature occurred as the source traversed the region of minor image perturbations lying between the pair of planetary caustics. Results. The estimated masses of the host and planet, their mass ratios, and the distance to the discovered planetary systems are (Mhost/M⊙, Mplanet/MJ, q/10−3, DL/kpc) = (0.58−0.30+0.33, 10.71−5.61+6.17, 17.61 ± 2.25, 6.67−1.30+0.93) for KMT-2020-BLG-0757, (0.53−0.31+0.31, 1.12−0.65+0.65, 2.01 ± 0.07, 6.66−1.84+1.19) for KMT-2022-BLG-0732, (0.42−0.23+0.32, 6.64−3.64+4.98, 15.07 ± 0.86, 7.55−1.30+0.89) for KMT-2022-BLG-1787, and (0.32−0.19+0.34, 4.98−2.94+5.42, 8.74 ± 0.49, 6.27−1.15+0.90) for KMT-2022-BLG-1852. These parameters indicate that all the planets are giants with masses exceeding the mass of Jupiter in our solar system and the hosts are low-mass stars with masses substantially less massive than the Sun.

AB - Aims. We investigated the nature of the anomalies appearing in four microlensing events KMT-2020-BLG-0757, KMT-2022-BLG-0732, KMT-2022-BLG-1787, and KMT-2022-BLG-1852. The light curves of these events commonly exhibit initial bumps followed by subsequent troughs that extend across a substantial portion of the light curves. Methods. We performed thorough modeling of the anomalies to elucidate their characteristics. Despite their prolonged durations, which differ from the usual brief anomalies observed in typical planetary events, our analysis revealed that each anomaly in these events originated from a planetary companion located within the Einstein ring of the primary star. It was found that the initial bump arouse when the source star crossed one of the planetary caustics, while the subsequent trough feature occurred as the source traversed the region of minor image perturbations lying between the pair of planetary caustics. Results. The estimated masses of the host and planet, their mass ratios, and the distance to the discovered planetary systems are (Mhost/M⊙, Mplanet/MJ, q/10−3, DL/kpc) = (0.58−0.30+0.33, 10.71−5.61+6.17, 17.61 ± 2.25, 6.67−1.30+0.93) for KMT-2020-BLG-0757, (0.53−0.31+0.31, 1.12−0.65+0.65, 2.01 ± 0.07, 6.66−1.84+1.19) for KMT-2022-BLG-0732, (0.42−0.23+0.32, 6.64−3.64+4.98, 15.07 ± 0.86, 7.55−1.30+0.89) for KMT-2022-BLG-1787, and (0.32−0.19+0.34, 4.98−2.94+5.42, 8.74 ± 0.49, 6.27−1.15+0.90) for KMT-2022-BLG-1852. These parameters indicate that all the planets are giants with masses exceeding the mass of Jupiter in our solar system and the hosts are low-mass stars with masses substantially less massive than the Sun.

KW - Planets and satellites: detection

KW - Gravitational lensing: micro

UR - https://ui.adsabs.harvard.edu/abs/2024arXiv240610547H/abstract

U2 - 10.1051/0004-6361/202450221

DO - 10.1051/0004-6361/202450221

M3 - Article

SN - 0004-6361

VL - 687

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - A225

ER -

Four microlensing giant planets detected through signals produced by minor-image perturbations

Abstract

Keywords

Access to Document

Handle.net

Other files and links

Fingerprint

ORP: Opticon RadioNet Pilot: ORP: Opticon RadioNet Pilot

Cite this

Four microlensing giant planets detected through signals produced by minor-image perturbations

Abstract

Keywords

Access to Document

Handle.net

Other files and links

Fingerprint

Projects

ORP: Opticon RadioNet Pilot: ORP: Opticon RadioNet Pilot

Cite this