Systematic KMTNet Planetary Anomaly Search, Paper I: OGLE-2019-BLG-1053Lb, A Buried Terrestrial Planet

Autor: Zang, Weicheng, Hwang, Kyu-Ha, Udalski, Andrzej, Wang, Tianshu, Zhu, Wei, Sumi, Takahiro, Yee, Jennifer C., Gould, Andrew, Mao, Shude, Zhang, Xiangyu, Albrow, Michael D., Chung, Sun-Ju, Han, Cheongho, Jung, Youn Kil, Ryu, Yoon-Hyun, Shin, In-Gu, Shvartzvald, Yossi, Cha, Sang-Mok, Kim, Dong-Jin, Kim, Hyoun-Woo, Kim, Seung-Lee, Lee, Chung-Uk, Lee, Dong-Joo, Lee, Yongseok, Park, Byeong-Gon, Pogge, Richard W., Mróz, Przemek, Skowron, Jan, Szymański, Michał K., Soszyński, Igor, Pietrukowicz, Paweł, Kozłowski, Szymon, Ulaczyk, Krzysztof, Rybicki, Krzysztof A., Iwanek, Patryk, Wrona, Marcin, Gromadzki, Mariusz, Bond, Ian A., Abe, Fumio, Barry, Richard, Bennett, David P., Bhattacharya, Aparna, Donachie, Martin, Fujii, Hirosane, Fukui, Akihiko, Hirao, Yuki, Itow, Yoshitaka, Kirikawa, Rintaro, Kondo, Iona, Koshimoto, Naoki, Li, Man Cheung Alex, Matsubara, Yutaka, Muraki, Yasushi, Miyazaki, Shota, Olmschenk, Greg, Ranc, Clément, Rattenbury, Nicholas J., Satoh, Yuki, Shoji, Hikaru, Silva, Stela Ishitani, Suzuki, Daisuke, Tanaka, Yuzuru, Tristram, Paul J., Yamawaki, Tsubasa, Yonehara, Atsunori, Beichman, Charles A., Bryden, Geoffery, Novati, Sebastiano Calchi, Carey, Sean, Gaudi, B. Scott, Henderson, Calen B., Johnson, Samson
Rok vydání: 2021
Předmět:
Druh dokumentu: Working Paper
DOI: 10.3847/1538-3881/ac12d4
Popis: In order to exhume the buried signatures of "missing planetary caustics" in the KMTNet data, we conducted a systematic anomaly search to the residuals from point-source point-lens fits, based on a modified version of the KMTNet EventFinder algorithm. This search reveals the lowest mass-ratio planetary caustic to date in the microlensing event OGLE-2019-BLG-1053, for which the planetary signal had not been noticed before. The planetary system has a planet-host mass ratio of $q = (1.25 \pm 0.13) \times 10^{-5}$. A Bayesian analysis yields estimates of the mass of the host star, $M_{\rm host} = 0.61_{-0.24}^{+0.29}~M_\odot$, the mass of its planet, $M_{\rm planet} = 2.48_{-0.98}^{+1.19}~M_{\oplus}$, the projected planet-host separation, $a_\perp = 3.4_{-0.5}^{+0.5}$ au, and the lens distance of $D_{\rm L} = 6.8_{-0.9}^{+0.6}$ kpc. The discovery of this very low mass-ratio planet illustrates the utility of our method and opens a new window for a large and homogeneous sample to study the microlensing planet-host mass-ratio function down to $q \sim 10^{-5}$.
Comment: published by AJ
Databáze: arXiv
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