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

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dc.contributor.authorHan, Cheongho
dc.contributor.authorBond, Ian A.
dc.contributor.authorLee, Chung-Uk
dc.contributor.authorGould, Andrew
dc.contributor.authorAlbrow, Michael D.
dc.contributor.authorChung, Sun-Ju
dc.contributor.authorHwang, Kyu-Ha
dc.contributor.authorJung, Youn Kil
dc.contributor.authorRyu, Yoon-Hyun
dc.contributor.authorShvartzvald, Yossi
dc.contributor.authorShin, In-Gu
dc.contributor.authorYee, Jennifer C.
dc.contributor.authorYang, Hongjing
dc.contributor.authorZang, Weicheng
dc.contributor.authorCha, Sang-Mok
dc.contributor.authorKim, Doeon
dc.contributor.authorKim, Dong-Jin
dc.contributor.authorKim, Seung-Lee
dc.contributor.authorLee, Dong-Joo
dc.contributor.authorLee, Yongseok
dc.contributor.authorPark, Byeong-Gon
dc.contributor.authorPogge, Richard W.
dc.contributor.authorAbe, Fumio
dc.contributor.authorBando, Ken
dc.contributor.authorBarry, Richard
dc.contributor.authorBennett, David P.
dc.contributor.authorBhattacharya, Aparna
dc.contributor.authorFujii, Hirosame
dc.contributor.authorFukui, Akihiko
dc.contributor.authorHamada, Ryusei
dc.contributor.authorHamada, Shunya
dc.contributor.authorHamasaki, Naoto
dc.contributor.authorHirao, Yuki
dc.contributor.authorIshitani Silva, Stela
dc.contributor.authorItow, Yoshitaka
dc.contributor.authorKirikawa, Rintaro
dc.contributor.authorKoshimoto, Naoki
dc.contributor.authorMatsubara, Yutaka
dc.contributor.authorMiyazaki, Shota
dc.contributor.authorMuraki, Yasushi
dc.contributor.authorNagai, Tutumi
dc.contributor.authorNunota, Kansuke
dc.contributor.authorOlmschenk, Greg
dc.contributor.authorRanc, Clement
dc.contributor.authorRattenbury, Nicholas J.
dc.contributor.authorSatoh, Yuki
dc.contributor.authorSumi, Takahiro
dc.contributor.authorSuzuki, Daisuke
dc.contributor.authorTomoyoshi, Mio
dc.contributor.authorTristram, Paul J.
dc.contributor.authorVandorou, Aikaterini
dc.contributor.authorYama, Hibiki
dc.contributor.authorYamashita, Kansuke
dc.contributor.authorBachelet, Etienne
dc.contributor.authorRota, Paolo
dc.contributor.authorBozza, Valerio
dc.contributor.authorZielinski, Pawel
dc.contributor.authorStreet, Rachel A.
dc.contributor.authorTsapras, Yiannis
dc.contributor.authorHundertmark, Markus
dc.contributor.authorWambsganss, Joachim
dc.contributor.authorWyrzykowski, Lukasz
dc.contributor.authorFiguera Jaimes, Roberto
dc.contributor.authorCassan, Arnaud
dc.contributor.authorDominik, Martin
dc.contributor.authorRybicki, Krzysztof A.
dc.contributor.authorRabus, Markus
dc.date.accessioned2025-01-20T16:12:53Z
dc.date.available2025-01-20T16:12:53Z
dc.date.issued2024
dc.description.abstractAims. 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-circle dot, 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.
dc.fuente.origenWOS
dc.identifier.doi10.1051/0004-6361/202450221
dc.identifier.eissn1432-0746
dc.identifier.issn0004-6361
dc.identifier.urihttps://doi.org/10.1051/0004-6361/202450221
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/90360
dc.identifier.wosidWOS:001269460100016
dc.language.isoen
dc.revistaAstronomy & astrophysics
dc.rightsacceso restringido
dc.subjectgravitational lensing: micro
dc.subjectplanets and satellites: general
dc.subject.ods13 Climate Action
dc.subject.odspa13 Acción por el clima
dc.titleFour microlensing giant planets detected through signals produced by minor-image perturbations
dc.typeartículo
dc.volumen687
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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