Han CBond IALee C-UGould AAlbrow MDChung S-JHwang K-HJung YKRyu Y-HShvartzvald YShin I-GYee JCYang HZang WCha S-MKim DKim D-JKim S-LLee D-JLee YPark B-GPogge RWAbe FBando KBarry RBennett DPBhattacharya AFujii HFukui AHamada RHamada SHamasaki NHirao YSilva SIItow YKirikawa RKoshimoto NMatsubara YMiyazaki SMuraki YNagai TNunota KOlmschenk GRanc CRattenbury NJSatoh YSumi TSuzuki DTomoyoshi MTristram PJVandorou AYama HYamashita KBachelet ERota PBozza VZielinski PStreet RATsapras YHundertmark MWambsganss JWyrzykowski ŁJaimes RFCassan ADominik MRybicki KARabus M2024-11-212024-11-212024-07Han C, Bond IA, Lee CU, Gould A, Albrow MD, Chung SJ, Hwang KH, Jung YK, Ryu YH, Shvartzvald Y, Shin IG, Yee JC, Yang H, Zang W, Cha SM, Kim D, Kim DJ, Kim SL, Lee DJ, Lee Y, Park BG, 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 and Astrophysics. 687. July 2024.0004-6361https://mro.massey.ac.nz/handle/10179/72044Aims. 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−+00.3033, 10.71−+56.6117, 17.61 ± 2.25, 6.67+−01.9330) for KMT-2020-BLG-0757, (0.53+−00.3131, 1.12+−00.6565, 2.01 ± 0.07, 6.66+−11.1984) for KMT-2022-BLG-0732, (0.42−+00.2332, 6.64−+43.9864, 15.07 ± 0.86, 7.55+−01.8930) for KMT-2022-BLG-1787, and (0.32+−00.3419, 4.98+−52.4294, 8.74 ± 0.49, 6.27+−01.9015) 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.(c) 2024 The Author/sCC BY 4.0https://creativecommons.org/licenses/by/4.0/gravitational lensingmicro – planets and satellitesgeneralJournal article10.1051/0004-6361/2024502211432-0746journal-articleA225