Four binary microlenses with directly measured masses
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arXiv
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| Formato: | Preprint |
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2025
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| author | Han, Cheongho Udalski, Andrzej Lee, Chung-Uk Bond, Ian A. Albrow, Michael D. Chung, Sun-Ju Gould, Andrew Jung, Youn Kil Hwang, Kyu-Ha Ryu, Yoon-Hyun Shvartzvald, Yossi Shin, In-Gu Yee, Jennifer C. Zang, Weicheng Yang, Hongjing Cha, Sang-Mok Kim, Doeon Kim, Dong-Jin Kim, Seung-Lee Lee, Dong-Joo Lee, Yongseok Park, Byeong-Gon Pogge, Richard W. Mróz, Przemek Szymański, Michał K. Skowron, Jan Poleski, Radosław Soszyński, Igor Pietrukowicz, Paweł Kozłowski, Szymon Rybicki, Krzysztof A. Iwanek, Patryk Ulaczyk, Krzysztof Wrona, Marcin Gromadzki, Mariusz Mróz, Mateusz J. Jaroszyński, Michał Kiraga, Marcin Abe, Fumio Bennett, David P. Bhattacharya, Aparna Fukui, Akihiko Hamada, Ryusei Silva, Stela Ishitani Hirao, Yuki Koshimoto, Naoki Matsubara, Yutaka Miyazaki, Shota Muraki, Yasushi Nagai, Tutumi Nunota, Kansuke Olmschenk, Greg Ranc, Clément Rattenbury, Nicholas J. Satoh, Yuki Sumi, Takahiro Suzuki, Daisuke Terry, Sean K. Tristram, Paul J. Vandorou, Aikaterini Yama, Hibiki |
| author_facet | Han, Cheongho Udalski, Andrzej Lee, Chung-Uk Bond, Ian A. Albrow, Michael D. Chung, Sun-Ju Gould, Andrew Jung, Youn Kil Hwang, Kyu-Ha Ryu, Yoon-Hyun Shvartzvald, Yossi Shin, In-Gu Yee, Jennifer C. Zang, Weicheng Yang, Hongjing Cha, Sang-Mok Kim, Doeon Kim, Dong-Jin Kim, Seung-Lee Lee, Dong-Joo Lee, Yongseok Park, Byeong-Gon Pogge, Richard W. Mróz, Przemek Szymański, Michał K. Skowron, Jan Poleski, Radosław Soszyński, Igor Pietrukowicz, Paweł Kozłowski, Szymon Rybicki, Krzysztof A. Iwanek, Patryk Ulaczyk, Krzysztof Wrona, Marcin Gromadzki, Mariusz Mróz, Mateusz J. Jaroszyński, Michał Kiraga, Marcin Abe, Fumio Bennett, David P. Bhattacharya, Aparna Fukui, Akihiko Hamada, Ryusei Silva, Stela Ishitani Hirao, Yuki Koshimoto, Naoki Matsubara, Yutaka Miyazaki, Shota Muraki, Yasushi Nagai, Tutumi Nunota, Kansuke Olmschenk, Greg Ranc, Clément Rattenbury, Nicholas J. Satoh, Yuki Sumi, Takahiro Suzuki, Daisuke Terry, Sean K. Tristram, Paul J. Vandorou, Aikaterini Yama, Hibiki |
| contents | We investigated binary lens events from the 2022-2024 microlensing surveys, aiming to identify events suitable for lens mass measurements. We focused on two key light curve features: distinct caustic spikes with resolved crossings for measuring the angular Einstein radius ($θ_{\rm E}$), and long durations enabling microlens-parallax ($π_{\rm E}$) measurements. Four events met these criteria: KMT-2022-BLG-1479, KMT-2023-BLG-0932, OGLE-2024-BLG-0142, and KMT-2024-BLG-1309. We estimated the angular Einstein radius by combining the normalized source radius measured from modeling the resolved caustic spikes with the angular source radius derived from the source color and magnitude. Additionally, we determined the microlens parallax through light curve modeling, considering higher-order effects caused by the orbital motions of Earth and the binary lens. With measurements of the event timescale, angular Einstein radius, and microlens parallax, we uniquely determined the mass and distance of the lens. For the events KMT-2022-BLG-1479, KMT-2023-BLG-0932, and KMT-2024-BLG-1309, both components of the binary lens have masses lower than that of the Sun, consistent with M-type dwarfs, which are the most common type of lenses in Galactic microlensing events. These lenses are relatively nearby, with distances $\lesssim 2.5$ kpc, indicating their location within the Galactic disk. In contrast, for OGLE-2024-BLG-0142, the primary lens component has a mass similar to that of the Sun, while the companion lens component has about half the mass of the primary. This lens system is situated at a greater distance, roughly 4.5 kpc. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2508_11079 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Four binary microlenses with directly measured masses Han, Cheongho Udalski, Andrzej Lee, Chung-Uk Bond, Ian A. Albrow, Michael D. Chung, Sun-Ju Gould, Andrew Jung, Youn Kil Hwang, Kyu-Ha Ryu, Yoon-Hyun Shvartzvald, Yossi Shin, In-Gu Yee, Jennifer C. Zang, Weicheng Yang, Hongjing Cha, Sang-Mok Kim, Doeon Kim, Dong-Jin Kim, Seung-Lee Lee, Dong-Joo Lee, Yongseok Park, Byeong-Gon Pogge, Richard W. Mróz, Przemek Szymański, Michał K. Skowron, Jan Poleski, Radosław Soszyński, Igor Pietrukowicz, Paweł Kozłowski, Szymon Rybicki, Krzysztof A. Iwanek, Patryk Ulaczyk, Krzysztof Wrona, Marcin Gromadzki, Mariusz Mróz, Mateusz J. Jaroszyński, Michał Kiraga, Marcin Abe, Fumio Bennett, David P. Bhattacharya, Aparna Fukui, Akihiko Hamada, Ryusei Silva, Stela Ishitani Hirao, Yuki Koshimoto, Naoki Matsubara, Yutaka Miyazaki, Shota Muraki, Yasushi Nagai, Tutumi Nunota, Kansuke Olmschenk, Greg Ranc, Clément Rattenbury, Nicholas J. Satoh, Yuki Sumi, Takahiro Suzuki, Daisuke Terry, Sean K. Tristram, Paul J. Vandorou, Aikaterini Yama, Hibiki Instrumentation and Methods for Astrophysics Earth and Planetary Astrophysics Astrophysics of Galaxies Solar and Stellar Astrophysics We investigated binary lens events from the 2022-2024 microlensing surveys, aiming to identify events suitable for lens mass measurements. We focused on two key light curve features: distinct caustic spikes with resolved crossings for measuring the angular Einstein radius ($θ_{\rm E}$), and long durations enabling microlens-parallax ($π_{\rm E}$) measurements. Four events met these criteria: KMT-2022-BLG-1479, KMT-2023-BLG-0932, OGLE-2024-BLG-0142, and KMT-2024-BLG-1309. We estimated the angular Einstein radius by combining the normalized source radius measured from modeling the resolved caustic spikes with the angular source radius derived from the source color and magnitude. Additionally, we determined the microlens parallax through light curve modeling, considering higher-order effects caused by the orbital motions of Earth and the binary lens. With measurements of the event timescale, angular Einstein radius, and microlens parallax, we uniquely determined the mass and distance of the lens. For the events KMT-2022-BLG-1479, KMT-2023-BLG-0932, and KMT-2024-BLG-1309, both components of the binary lens have masses lower than that of the Sun, consistent with M-type dwarfs, which are the most common type of lenses in Galactic microlensing events. These lenses are relatively nearby, with distances $\lesssim 2.5$ kpc, indicating their location within the Galactic disk. In contrast, for OGLE-2024-BLG-0142, the primary lens component has a mass similar to that of the Sun, while the companion lens component has about half the mass of the primary. This lens system is situated at a greater distance, roughly 4.5 kpc. |
| title | Four binary microlenses with directly measured masses |
| topic | Instrumentation and Methods for Astrophysics Earth and Planetary Astrophysics Astrophysics of Galaxies Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2508.11079 |