Two Microlensing Planets through Planetary-Caustic Channel: Light Curve Analysis
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Authors:
(1) Youn Kil Jung, Korea Astronomy and Space Science Institute, University of Science and Technology, and The KMTNet Collaboration;
(2) Cheongho Han, Department of Physics, Chungbuk National University and The KMTNet Collaboration;
(3) Andrzej Udalski, Warsaw University Observatory and The OGLE Collaboration;
(4) Andrew Gould, Korea Astronomy and Space Science Institute, Department of Astronomy, Ohio State University, Max-Planck-Institute for Astronomy and The KMTNet Collaboration;
(5) Jennifer C. Yee, Center for Astrophysics | Harvard & Smithsonian and The KMTNet Collaboration;
(6) Michael D. Albrow, University of Canterbury, Department of Physics and Astronomy;
(7) Sun-Ju Chung, Korea Astronomy and Space Science Institute and University of Science and Technology;
(8) Kyu-Ha Hwang, Korea Astronomy and Space Science Institute;
(9) Yoon-Hyun Ryu, Korea Astronomy and Space Science Institute;
(10) In-Gu Shin, Korea Astronomy and Space Science Institute;
(11) Yossi Shvartzvald, Department of Particle Physics and Astrophysics, Weizmann Institute of Science;
(12) Wei Zhu, Canadian Institute for Theoretical Astrophysics, University of Toronto;
(13) Weicheng Zang, Department of Astronomy, Tsinghua University;
(14) Sang-Mok Cha, Korea Astronomy and Space Science Institute and 2School of Space Research, Kyung Hee University;
(15) Dong-Jin Kim, Korea Astronomy and Space Science Institute;
(16) Hyoun-Woo Kim, Korea Astronomy and Space Science Institute;
(17) Seung-Lee Kim, Korea Astronomy and Space Science Institute and University of Science and Technology;
(18) Chung-Uk Lee, Korea Astronomy and Space Science Institute and University of Science and Technology;
(19) Dong-Joo Lee, Korea Astronomy and Space Science Institute;
(20) Yongseok Lee, Korea Astronomy and Space Science Institute and School of Space Research, Kyung Hee University;
(21) Byeong-Gon Park, Korea Astronomy and Space Science Institute and University of Science and Technology;
(22) Richard W. Pogge, Department of Astronomy, Ohio State University;
(23) Przemek Mroz, Warsaw University Observatory and Division of Physics, Mathematics, and Astronomy, California Institute of Technology;
(24) Michal K. Szymanski, Warsaw University Observatory;
(25) Jan Skowron, Warsaw University Observatory;
(26) Radek Poleski, Warsaw University Observatory and Department of Astronomy, Ohio State University;
(27) Igor Soszynski, Warsaw University Observatory;
(28) Pawel Pietrukowicz, Warsaw University Observatory;
(29) Szymon Kozlowski, Warsaw University Observatory;
(30) Krzystof Ulaczyk, Department of Physics, University of Warwick, Gibbet;
(31) Krzysztof A. Rybicki, Warsaw University Observatory;
(32) Patryk Iwanek, Warsaw University Observatory;
(33) Marcin Wrona, Warsaw University Observatory.
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Table of Links
Abstract and Intro
Observation
Light Curve Analysis
Physical Parameters
Microlensing Planets in the (log s, log q) plane
Summary and Conclusions
References
3. Light Curve Analysis
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In Figures 3 and 4, we present the lens-system configurations of the individual events, showing the source trajectory with respect to the lens components and resulting caustics. From the configurations, it is found that the anomalies of both events are produced by the source crossing over the planetary caustic of the lens system. For OGLE-2018-BLG-0567, the source size is comparable to the caustic size, and thus the detailed caustic-crossing features, two caustic spikes and a U-shape trough region between the spikes, was smeared out by finite source effects. For OGLE-2018-BLG-0962, on the other hand, the caustic is much bigger than the source size, and thus detailed caustic-crossing feature of the anomaly is well delineated. It is found the first part of the anomaly, centered at HJD′ (= HJD − 2, 450, 000 days) ∼ 8271.5, was produced by the source passing over the two caustic segments that flank the inner cusp (on the binary axis) of the planetary caustic, and the second part, centered at HJD′ ∼ 8273.8, was generated by the source passage over the adjacent (off-axis) cusp.
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This paper is available on arxiv under CC0 1.0 DEED license.
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