OGLE-2019-BLG-0304: Competing Interpretations between a Planet–binary Model and a Binary-source + Binary-lens Model
- Creators
- Han, Cheongho
- Udalski, Andrzej
- Lee, Chung-Uk
- Kim, Doeon
- Ryu, Yoon-Hyun
- Albrow, Michael D.
- Chung, Sun-Ju
- Gould, Andrew
- Hwang, Kyu-Ha
- Kil Jung, Youn
- Kim, Hyoun-Woo
- Shin, In-Gu
- Shvartzvald, Yossi
- Yee, Jennifer C.
- Zang, Weicheng
- Cha, Sang-Mok
- Kim, Dong-Jin
- Kim, Seung-Lee
- Lee, Dong-Joo
- Lee, Yongseok
- Park, Byeong-Gon
- Pogge, Richard W.
- Mróz, Przemek
- Szymański, Michał K.
- Skowron, Jan
- Poleski, Radosław
- Soszyński, Igor
- Pietrukowicz, Paweł
- Kozłowski, Szymon
- Ulaczyk, Krzysztof
- Rybicki, Krzysztof A.
- Iwanek, Patryk
- Wrona, Marcin
- Gromadzki, Mariusz
- KMTNet Collaboration
- OGLE Collaboration
Abstract
We analyze the microlensing event OGLE-2019-BLG-0304, whose light curve exhibits two distinctive features: a deviation in the peak region and a second bump appearing ∼61 days after the main peak. Although a binary-lens model can explain the overall features, it leaves subtle but noticeable residuals in the peak region. We find that the residuals can be explained by the presence of either a planetary companion located close to the primary of the binary lens (3L1S model) or an additional close companion to the source (2L2S model). Although the 3L1S model is favored over the 2L2S model, with Δχ² ∼ 8, securely resolving the degeneracy between the two models is difficult with the currently available photometric data. According to the 3L1S interpretation, the lens is a planetary system, in which a planet with a mass 0.51^(+0.51)_(−0.23) M_J is in an S-type orbit around a binary composed of stars with masses 0.27^(+0.27)_(−0.12) M_⊙ and 0.10^(+0.10)_(−0.04) M_⊙. According to the 2L2S interpretation, however, the source is composed of G- and K-type giant stars and the lens is composed of a low-mass M dwarf and a brown dwarf with masses 0.12^(+0.12)_(−0.05) M_⊙ and 0.045^(+0.045)_(−.019), respectively. The event illustrates the need for thorough model testing in the interpretation of lensing events with complex features in light curves.
Additional Information
© 2021. The American Astronomical Society. Received 2021 March 11; revised 2021 August 2; accepted 2021 August 7; published 2021 October 19. Work by C.H. was supported by grants from the National Research Foundation of Korea (2019 R1A2C2085965 and 2020 R1A4A2002885). Work by A.G. was supported by JPL grant 1500811. 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. The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to AU.Attached Files
Published - Han_2021_AJ_162_203.pdf
Accepted Version - 2109.02209.pdf
Files
Name | Size | Download all |
---|---|---|
md5:76d4a186bddd1b922c5e4c97f5753766
|
2.2 MB | Preview Download |
md5:63dfcf3b9628123d8aff382314071fc9
|
2.0 MB | Preview Download |
Additional details
- Eprint ID
- 111824
- Resolver ID
- CaltechAUTHORS:20211110-164935957
- 2019 R1A2C2085965
- National Research Foundation of Korea
- 2020 R1A4A2002885
- National Research Foundation of Korea
- 1500811
- JPL
- MAESTRO 2014/14/A/ST9/00121
- National Science Centre (Poland)
- Created
-
2021-11-11Created from EPrint's datestamp field
- Updated
-
2021-11-11Created from EPrint's last_modified field