OGLE-2017-BLG-0482Lb: A Microlensing Super-Earth Orbiting a Low-mass Host Star
journal contribution
posted on 2019-09-24, 16:24 authored by C Han, Y Hirao, A Udalski, CU Lee, V Bozza, A Gould, F Abe, R Barry, IA Bond, DP Bennett, A Bhattacharya, M Donachie, P Evans, A Fukui, Y Itow, K Kawasaki, N Koshimoto, MCA Li, CH Ling, Y Matsubara, S Miyazaki, H Munakata, Y Muraki, M Nagakane, K Ohnishi, C Ranc, N Rattenbury, T Saito, A Sharan, DJ Sullivan, T Sumi, D Suzuki, PJ Tristram, T Yamada, A Yonehara, P Mróz, R Poleski, S Kozłowski, I Soszyński, P Pietrukowicz, J Skowron, MK Szymański, K Ulaczyk, M Pawlak, K Rybicki, P Iwanek, MD Albrow, SJ Chung, KH Hwang, YK Jung, D Kim, WT Kim, HW Kim, YH Ryu, IG Shin, Y Shvartzvald, JC Yee, W Zhu, SM Cha, SL Kim, DJ Kim, DJ Lee, Y Lee, BG Park, RW PoggeWe report the discovery of a planetary system in which a super-Earth orbits a late M-dwarf host. The planetary system was found from the analysis of the microlensing event OGLE-2017-BLG-0482, wherein the planet signal appears as a short-term anomaly to the smooth lensing light curve produced by the host. Despite its weak signal and short duration, the planetary signal was firmly detected from the dense and continuous coverage by three microlensing surveys. We find a planet/host mass ratio of q ∼ 1.4 × 10-4. We measure the microlens parallax from the long-term deviation in the observed lensing light curve, but the angular Einstein radius cannot be measured because the source trajectory did not cross the planet-induced caustic. Using the measured event timescale and the microlens parallax, we find that the masses of the planet and the host are and , respectively, and the projected separation between them is au. The estimated distance to the lens is kpc. The discovery of the planetary system demonstrates that microlensing provides an important method to detect low-mass planets orbiting low-mass stars.
Funding
Work by C.H. was supported by the grant (2017R1A4A1015178) of National Research Foundation of Korea. The MOA project is supported by JSPS KAKENHI grant Nos. JSPS24253004, JSPS26247023, JSPS23340064, JSPS15H00781, and JP16H06287. The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U. Work by A.G. was supported by JPL grant 1500811. Work by J.C.Y. was performed under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. Work by Y.S. was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Universities Space Research Association through a contract with NASA. We acknowledge the high-speed internet service (KREONET) provided by Korea Institute of Science and Technology Information (KISTI). 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.
History
Citation
Astronomical Journal, 2018, 155 (5)Author affiliation
/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and AstronomyVersion
- VoR (Version of Record)
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Astronomical JournalPublisher
American Astronomical Society, IOP Publishingissn
0004-6256Acceptance date
2018-03-27Copyright date
2018Available date
2019-09-24Publisher DOI
Publisher version
https://iopscience.iop.org/article/10.3847/1538-3881/aabad2Language
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