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KMT-2019-BLG-1715: planetary microlensing event with three lens masses and two source stars

Han, Cheongho and Udalski, Andrzej and Kim, Doeone and Jung, Youn Kil and Lee, Chung-Uk and Bond, Ian A. and Albrow, Michael D. and Chung, Sun-Ju and Gould, Andrew and Hwang, Kyu-Ha and Kim, Hyoun-Woo and Ryu, Yoon-Hyun and Shin, In-Gu and Shvartzvald, Yossi and Zang, Weicheng and Yee, Jennifer C. and Cha, Sang-Mok and Kim, Dong-Jin and Kim, Seung-Lee and Lee, Dong-Joo and Lee, Yongseok and Park, Byeong-Gon and Pogge, Richard W. and Kim, Chun-Hwey and Kim, Woong-Tae and Mróz, Przemek and Szymański, Michał K. and Skowron, Jan and Poleski, Radek and Soszyński, Igor and Pietrukowicz, Paweł and Kozłowski, Szymon and Ulaczyk, Krzysztof and Rybicki, Krzysztof A. and Iwanek, Patryk and Wrona, Marcin and Gromadzki, Mariusz and Abe, Fumio and Barry, Richard and Bennett, David P. and Bhattacharya, Aparna and Donachie, Martin and Fujii, Hirosane and Fukui, Akihiko and Itow, Yoshitaka and Hirao, Yuki and Kirikawa, Rintaro and Kondo, Iona and Li, Man Cheung Alex and Matsubara, Yutaka and Muraki, Yasushi and Miyazaki, Shota and Ranc, Clément and Rattenbury, Nicholas J. and Satoh, Yuki and Shoji, Hikaru and Suematsu, Haruno and Sumi, Takahiro and Suzuki, Daisuke and Tanaka, Yuzuru and Tristram, Paul J. and Yamakawa, Takeharu and Yamawaki, Tsubasa and Yonehara, Atsunori (2021) KMT-2019-BLG-1715: planetary microlensing event with three lens masses and two source stars. . (Unpublished)

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We investigate the gravitational microlensing event KMT-2019-BLG-1715, of which light curve shows two short-term anomalies from a caustic-crossing binary-lensing light curve: one with a large deviation and the other with a small deviation. We identify five pairs of solutions, in which the anomalies are explained by adding an extra lens or source component in addition to the base binary-lens model. We resolve the degeneracies by applying a method, in which the measured flux ratio between the first and second source stars is compared with the flux ratio deduced from the ratio of the source radii. Applying this method leaves a single pair of viable solutions, in both of which the major anomaly is generated by a planetary-mass third body of the lens, and the minor anomaly is generated by a faint second source. A Bayesian analysis indicates that the lens comprises three masses: a planet-mass object with ∼2.6 M_J and binary stars of K and M dwarfs lying in the galactic disk. We point out the possibility that the lens is the blend, and this can be verified by conducting high-resolution followup imaging for the resolution of the lens from the source.

Item Type:Report or Paper (Discussion Paper)
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URLURL TypeDescription Paper
Han, Cheongho0000-0002-2641-9964
Mróz, Przemek0000-0001-7016-1692
Additional Information:Attribution 4.0 International (CC BY 4.0). Work by C.H. was supported by the grants of National Research Foundation of Korea (2020R1A4A2002885 and 2019R1A2C2085965) Work by A.G. was supported by JPL grant 1500811. 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 was supported by the grant 19KK0082 and 20H04754. Work by Y.H, was supported by JSPS KAKENHI grant No. 17J02146. D.P.B., A.B., and C.R. were supported by NASA through grant NASA-80NSSC18K0274. Work by N.K. was supported by JSPS KAKENHI grant No. JP18J008. Work by C.R. was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by USRA through a contractwith NASA. This research hasmade 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.
Funding AgencyGrant Number
National Research Foundation of Korea2020R1A4A2002885
National Research Foundation of Korea2019R1A2C2085965
National Science Centre (Poland)MAESTRO 2014/14/A/ST9/00121
Japan Society for the Promotion of Science (JSPS)19KK0082
Japan Society for the Promotion of Science (JSPS)20H04754
Japan Society for the Promotion of Science (JSPS)17J02146
Japan Society for the Promotion of Science (JSPS)JP18J00897
NASA Postdoctoral ProgramUNSPECIFIED
Record Number:CaltechAUTHORS:20210409-141511091
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:108679
Deposited By: Tony Diaz
Deposited On:12 Apr 2021 01:26
Last Modified:12 Apr 2021 01:26

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