Systematic KMTNet Planetary Anomaly Search. II. Six New q < 2 × 10⁻⁴ Mass-ratio Planets
- Creators
- Hwang, Kyu-Ha
- Zang, Weicheng
- Gould, Andrew
- Udalski, Andrzej
- Bond, Ian A.
- Yang, Hongjing
- Mao, Shude
- Albrow, Michael D.
- Chung, Sun-Ju
- Han, Cheongho
- Jung, Youn Kil
- Ryu, Yoon-Hyun
- Shin, In-Gu
- Shvartzvald, Yossi
- Yee, Jennifer C.
- 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
- Poleski, Radek
- Skowron, Jan
- Szymanski, Michal K.
- Soszyński, Igor
- Pietrukowicz, Pawel
- Kozlowski, Szymon
- Ulaczyk, Krzysztof
- Rybicki, Krzysztof A.
- Iwanek, Patryk
- Wrona, Marcin
- Gromadzki, Mariusz
- Abe, Fumio
- Barry, Richard
- Bennett, David P.
- Bhattacharya, Aparna
- Fujii, Hirosame
- Fukui, Akihiko
- Hirao, Yuki
- Itow, Yoshitaka
- Kirikawa, Rintaro
- Kondo, Iona
- Koshimoto, Naoki
- Munford, Brandon
- Matsubara, Yutaka
- Miyazaki, Shota
- Muraki, Yasushi
- Olmschenk, Greg
- Ranc, Clément
- Rattenbury, Nicholas J.
- Satoh, Yuki K.
- Shoji, Hikaru
- Silva, Stela Ishitani
- Sumi, Takahiro
- Suzuki, Daisuke
- Tristram, Paul J.
- Yonehara, Atsunori
- Zhang, Xiangyu
- Zhu, Wei
- Penny, Matthew T.
- Fouqué, Pascal
- KMTNet Collaboration
- OGLE Collaboration
- MOA Collaboration
- Tsinghua and CFHT Microlensing Group
Abstract
We 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 −5 < log q < −3.7. 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.
Additional Information
© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2021 June 11; revised 2021 November 3; accepted 2021 November 3; published 2022 January 5. This research has made use of the KMTNet system operated by the Korea Astronomy and Space Science Institute (KASI), and the data were obtained at three host sites of CTIO in Chile, SAAO in South Africa, and SSO in Australia. Work by C.H. was supported by the grants of the National Research Foundation of Korea (2019R1A2C2085965 and 2020R1A4A2002885). The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U. The MOA project is supported by JSPS KAKENHI grant Nos. JSPS24253004, JSPS26247023, JSPS23340064, JSPS15H00781, and JP16H06287. W.Z., S.M., X.Z., and H.Y. acknowledge support by the National Science Foundation of China (grant Nos. 11821303 and 11761131004). This research uses data obtained through the Telescope Access Program (TAP), which has been funded by the TAP member institutes. We are very grateful to the instrumentation and operations teams at CFHT that fixed several failures of MegaCam in the shortest time possible, allowing its return onto the telescope and these crucial observations.Attached Files
Published - Hwang_2022_AJ_163_43.pdf
Submitted - 2106.06686.pdf
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Additional details
- Eprint ID
- 112236
- Resolver ID
- CaltechAUTHORS:20211206-214713430
- 2019R1A2C2085965
- National Research Foundation of Korea
- 2020R1A4A2002885
- National Research Foundation of Korea
- MAESTRO 2014/14/A/ST9/00121
- National Science Centre (Poland)
- JSPS24253004
- Japan Society for the Promotion of Science (JSPS)
- JSPS26247023
- Japan Society for the Promotion of Science (JSPS)
- JSPS23340064
- Japan Society for the Promotion of Science (JSPS)
- JSPS15H00781
- Japan Society for the Promotion of Science (JSPS)
- JP16H06287
- Japan Society for the Promotion of Science (JSPS)
- 11821303
- National Natural Science Foundation of China
- 11761131004
- National Natural Science Foundation of China
- TAP member institutes
- Created
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2021-12-07Created from EPrint's datestamp field
- Updated
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2022-01-24Created from EPrint's last_modified field