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Four microlensing giant planets detected through signals produced by minor-image perturbations
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dc.contributor.author | Han, Cheongho | |
dc.contributor.author | Bond, Ian A. | |
dc.contributor.author | Lee, Chung-Uk | |
dc.contributor.author | Gould, Andrew | |
dc.contributor.author | Albrow, Michael D. | |
dc.contributor.author | Chung, Sun-Ju | |
dc.contributor.author | Hwang, Kyu-Ha | |
dc.contributor.author | Jung, Youn Kil | |
dc.contributor.author | Ryu, Yoon-Hyun | |
dc.contributor.author | Shvartzvald, Yossi | |
dc.contributor.author | Shin, In-Gu | |
dc.contributor.author | Yee, Jennifer C. | |
dc.contributor.author | Yang, Hongjing | |
dc.contributor.author | Zang, Weicheng | |
dc.contributor.author | Cha, Sang-Mok | |
dc.contributor.author | Kim, Doeon | |
dc.contributor.author | Kim, Dong-Jin | |
dc.contributor.author | Kim, Seung-Lee | |
dc.contributor.author | Lee, Dong-Joo | |
dc.contributor.author | Lee, Yongseok | |
dc.contributor.author | Park, Byeong-Gon | |
dc.contributor.author | Pogge, Richard W. | |
dc.contributor.author | Abe, Fumio | |
dc.contributor.author | Bando, Ken | |
dc.contributor.author | Barry, Richard | |
dc.contributor.author | Bennett, David P. | |
dc.contributor.author | Bhattacharya, Aparna | |
dc.contributor.author | Fujii, Hirosame | |
dc.contributor.author | Fukui, Akihiko | |
dc.contributor.author | Hamada, Ryusei | |
dc.contributor.author | Hamada, Shunya | |
dc.contributor.author | Hamasaki, Naoto | |
dc.contributor.author | Hirao, Yuki | |
dc.contributor.author | Silva, Stela Ishitani | |
dc.contributor.author | Itow, Yoshitaka | |
dc.contributor.author | Kirikawa, Rintaro | |
dc.contributor.author | Koshimoto, Naoki | |
dc.contributor.author | Matsubara, Yutaka | |
dc.contributor.author | Miyazaki, Shota | |
dc.contributor.author | Muraki, Yasushi | |
dc.contributor.author | Nagai, Tutumi | |
dc.contributor.author | Nunota, Kansuke | |
dc.contributor.author | Olmschenk, Greg | |
dc.contributor.author | Ranc, Clément | |
dc.contributor.author | Rattenbury, Nicholas J. | |
dc.contributor.author | Satoh, Yuki | |
dc.contributor.author | Sumi, Takahiro | |
dc.contributor.author | Suzuki, Daisuke | |
dc.contributor.author | Tomoyoshi, Mio | |
dc.contributor.author | Tristram, Paul J. | |
dc.contributor.author | Vandorou, Aikaterini | |
dc.contributor.author | Yama, Hibiki | |
dc.contributor.author | Yamashita, Kansuke | |
dc.contributor.author | Bachelet, Etienne | |
dc.contributor.author | Rota, Paolo | |
dc.contributor.author | Bozza, Valerio | |
dc.contributor.author | Zielinski, Paweł | |
dc.contributor.author | Street, Rachel A. | |
dc.contributor.author | Tsapras, Yiannis | |
dc.contributor.author | Hundertmark, Markus | |
dc.contributor.author | Wambsganss, Joachim | |
dc.contributor.author | Wyrzykowski, Łukasz | |
dc.contributor.author | Jaimes, Roberto Figuera | |
dc.contributor.author | Cassan, Arnaud | |
dc.contributor.author | Dominik, Martin | |
dc.contributor.author | Rybicki, Krzysztof A. | |
dc.contributor.author | Rabus, Markus | |
dc.date.accessioned | 2024-07-23T16:30:09Z | |
dc.date.available | 2024-07-23T16:30:09Z | |
dc.date.issued | 2024-07 | |
dc.identifier | 304163938 | |
dc.identifier | 3a0db12a-f0d7-4716-9298-5c584b3d9277 | |
dc.identifier.citation | 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 , Lee , Y , Park , B-G , Pogge , R W , Abe , F , Bando , K , Barry , R , Bennett , D P , Bhattacharya , A , Fujii , H , Fukui , A , Hamada , R , Hamada , S , Hamasaki , N , Hirao , Y , Silva , S I , Itow , Y , Kirikawa , R , Koshimoto , N , Matsubara , Y , Miyazaki , S , Muraki , Y , Nagai , T , Nunota , K , Olmschenk , G , Ranc , C , Rattenbury , N J , Satoh , Y , Sumi , T , Suzuki , D , Tomoyoshi , M , Tristram , P J , Vandorou , A , Yama , H , Yamashita , K , Bachelet , E , Rota , P , Bozza , V , Zielinski , P , Street , R A , Tsapras , Y , Hundertmark , M , Wambsganss , J , Wyrzykowski , Ł , Jaimes , R F , Cassan , A , Dominik , M , Rybicki , K A & 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 | en |
dc.identifier.issn | 0004-6361 | |
dc.identifier.other | ArXiv: http://arxiv.org/abs/2406.10547v1 | |
dc.identifier.other | ORCID: /0000-0002-3202-0343/work/163120780 | |
dc.identifier.uri | https://hdl.handle.net/10023/30256 | |
dc.description | 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. | en |
dc.description.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. | |
dc.format.extent | 10 | |
dc.format.extent | 2238085 | |
dc.language.iso | eng | |
dc.relation.ispartof | Astronomy & Astrophysics | en |
dc.subject | Planets and satellites: detection | en |
dc.subject | Gravitational lensing: micro | en |
dc.subject | QB Astronomy | en |
dc.subject | 3rd-NDAS | en |
dc.subject.lcc | QB | en |
dc.title | Four microlensing giant planets detected through signals produced by minor-image perturbations | en |
dc.type | Journal article | en |
dc.contributor.sponsor | European Commission | en |
dc.contributor.institution | University of St Andrews. School of Physics and Astronomy | en |
dc.contributor.institution | University of St Andrews. St Andrews Centre for Exoplanet Science | en |
dc.identifier.doi | https://doi.org/10.1051/0004-6361/202450221 | |
dc.description.status | Peer reviewed | en |
dc.identifier.url | https://ui.adsabs.harvard.edu/abs/2024arXiv240610547H/abstract | en |
dc.identifier.grantnumber | 101004719 | en |
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