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Two Microlensing Planets through Planetary-Caustic Channel: Physical Parametersby@exoplanetology

Two Microlensing Planets through Planetary-Caustic Channel: Physical Parameters

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In this paper, researchers analyze microlensing events OGLE-2018-BLG-0567 and OGLE-2018-BLG-0962, revealing planetary companions to the hosts.
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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.

4. Physical Parameters






The bulge VD is modeled based on stars in the Gaia catalog (Gaia Collaboration et al. 2016, 2018). That is, we first find red giant stars in the catalog within 2 arcmin centered on the event location. We then derive their mean velocity and its dispersion in Galactocentric Cartesian coordinates (x, y, z) as defined in Han & Gould (1995).




This paper is available on arxiv under CC0 1.0 DEED license.


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