Hwang K-HZang WGould AUdalski ABond IAYang HMao SAlbrow MDChung S-JHan CJung YKRyu Y-HShin I-GShvartzvald YYee JCCha S-MKim D-JKim H-WKim S-LLee C-ULee D-JLee YPark B-GPogge RMróz PPoleski RSkowron JSzymański MKSoszyński IPietrukowicz PKozłowski SUlaczyk KRybicki KAIwanek PWrona MGromadzki MAbe FBarry RBennett DPBhattacharya AFujii HFukui AHirao YItow YKirikawa RKondo IKoshimoto NMunford BMatsubara YMiyazaki SMuraki YOlmschenk GRanc CRattenbury NJSatoh YKShoji HSilva SISumi TSuzuki DTristram PJYonehara AZhang XZhu WPenny MTFouqué P2023-11-082023-11-202022-01-052023-11-082023-11-202022-02-01Hwang KH, Zang W, Gould A, Udalski A, Bond IA, Yang H, Mao S, Albrow MD, Chung SJ, Han C, Kil Jung Y, Ryu YH, Shin IG, Shvartzvald Y, Yee JC, Cha SM, Kim DJ, Kim HW, Kim SL, Lee CU, Lee DJ, Lee Y, Park BG, Pogge RW, Mróz P, Poleski R, Skowron J, Szymański MK, Soszyński I, Pietrukowicz P, Kozłowski S, Ulaczyk K, Rybicki KA, Iwanek P, Wrona M, Gromadzki M, Abe F, Barry R, Bennett DP, Bhattacharya A, Fujii H, Fukui A, Hirao Y, Itow Y, Kirikawa R, Kondo I, Koshimoto N, Munford B, Matsubara Y, Miyazaki S, Muraki Y, Olmschenk G, Ranc C, Rattenbury NJ, Satoh YK, Shoji H, Ishitani Silva S, Sumi T, Suzuki D, Tristram PJ, Yonehara A, Zhang X, Zhu W, Penny MT, Fouqué P. (2022). Systematic KMTNet Planetary Anomaly Search. II. Six New q &lt; 2 × 10^-4Mass-ratio Planets. Astronomical Journal. 163. 2.0004-6256https://mro.massey.ac.nz/handle/10179/69140We apply the automated AnomalyFinder algorithm of Paper I to 2018-2019 light curves from the ≃13 deg2 covered by the six KMTNet prime fields, with cadences Γ ≥ 2 hr-1. We find a total of 11 planets with mass ratios q < 2 × 10-4, including 6 newly discovered planets, 1 planet that was reported in Paper I, and recovery of 4 previously discovered planets. One of the new planets, OGLE-2018-BLG-0977Lb, is in a planetary caustic event, while the other five (OGLE-2018-BLG-0506Lb, OGLE-2018-BLG-0516Lb, OGLE-2019-BLG-1492Lb, KMT-2019-BLG-0253, and KMT-2019-BLG-0953) are revealed by a "dip"in the light curve as the source crosses the host-planet axis on the opposite side of the planet. These subtle signals were missed in previous by-eye searches. The planet-host separations (scaled to the Einstein radius), s, and planet-host mass ratios, q, are, respectively, (s, q × 105) = (0.88, 4.1), (0.96 ± 0.10, 8.3), (0.94 ± 0.07, 13), (0.97 ± 0.07, 18), (0.97 ± 0.04, 4.1), and (0.74, 18), where the "± "indicates a discrete degeneracy. The 11 planets are spread out over the range . Together with the two planets previously reported with q ∼ 10-5 from the 2018-2019 nonprime KMT fields, this result suggests that planets toward the bottom of this mass-ratio range may be more common than previously believed.CC BY 4.0https://creativecommons.org/licenses/by/4.0/Gravitational microlensing exoplanet detection (2147)Journal article10.3847/1538-3881/ac38ad1538-3881journal-articlehttp://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000739048200001&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=c5bb3b2499afac691c2e3c1a83ef6fefARTN 43