The Astronomical Journal (Jan 2024)

OGLE-2017-BLG-0448Lb: A Low Mass–Ratio Wide-orbit Microlensing Planet?

  • Ruocheng Zhai,
  • Radosław Poleski,
  • Weicheng Zang,
  • Youn Kil Jung,
  • Andrzej Udalski,
  • Renkun Kuang,
  • Leading Authors,
  • Michael D. Albrow,
  • Sun-Ju Chung,
  • Andrew Gould,
  • Cheongho Han,
  • Kyu-Ha Hwang,
  • Yoon-Hyun Ryu,
  • In-Gu Shin,
  • Yossi Shvartzvald,
  • Hongjing Yang,
  • Jennifer C. Yee,
  • Sang-Mok Cha,
  • Dong-Jin Kim,
  • Hyoun-Woo Kim,
  • Seung-Lee Kim,
  • Chung-Uk Lee,
  • Dong-Joo Lee,
  • Yongseok Lee,
  • Byeong-Gon Park,
  • Richard W. Pogge,
  • The KMTNet Collaboration,
  • Jan Skowron,
  • Michał K. Szymański,
  • Igor Soszyński,
  • Krzysztof Ulaczyk,
  • Paweł Pietrukowicz,
  • Szymon Kozłowski,
  • Przemek Mróz,
  • Krzysztof A. Rybicki,
  • Patryk Iwanek,
  • Marcin Wrona,
  • Mariusz Gromadzki,
  • The OGLE Collaboration,
  • Hanyue Wang,
  • Shude Mao,
  • Jiyuan Zhang,
  • Qiyue Qian,
  • Wei Zhu,
  • The MAP Collaboration

DOI
https://doi.org/10.3847/1538-3881/ad284f
Journal volume & issue
Vol. 167, no. 4
p. 162

Abstract

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The gravitational microlensing technique is most sensitive to planets in a Jupiter-like orbit and has detected more than 200 planets. However, only a few wide-orbit ( s > 2) microlensing planets have been discovered, where s is the planet-to-host separation normalized to the angular Einstein ring radius, θ _E . Here, we present the discovery and analysis of a strong candidate wide-orbit microlensing planet in the event OGLE-2017-BLG-0448. The whole light curve exhibits long-term residuals to the static binary-lens single-source model, so we investigate the residuals by adding the microlensing parallax, microlensing xallarap, an additional lens, or an additional source. For the first time, we observe a complex degeneracy between all four effects. The wide-orbit models with s ∼ 2.5 and a planet-to-host mass ratio of q ∼ 10 ^−4 are significantly preferred, but we cannot rule out the close models with s ∼ 0.35 and q ∼ 10 ^−3 . A Bayesian analysis based on a Galactic model indicates that, despite the complicated degeneracy, the surviving wide-orbit models all contain a super-Earth-mass to Neptune-mass planet at a projected planet-host separation of ∼6 au and the surviving close-orbit models all consist of a Jovian-mass planet at ∼1 au. The host star is probably an M or K dwarf. We discuss the implications of this dimension-degeneracy disaster on microlensing light-curve analysis and its potential impact on statistical studies.

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