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Journal Articles The Astronomical Journal Year : 2019

KMT-2017-BLG-0165Lb: A Super-Neptune-mass Planet Orbiting a Sun-like Host Star

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Youn Kil Jung
  • Function : Author
Andrew Gould
Weicheng Zang
  • Function : Author
Kyu-Ha Hwang
  • Function : Author
Yoon-Hyun Ryu
  • Function : Author
Cheongho Han
  • Function : Author
Jennifer C. Yee
  • Function : Author
Michael D. Albrow
  • Function : Author
Sun-Ju Chung
  • Function : Author
In-Gu Shin
  • Function : Author
Yossi Shvartzvald
  • Function : Author
Wei Zhu
  • Function : Author
Sang-Mok Cha
  • Function : Author
Dong-Jin Kim
  • Function : Author
Hyoun-Woo Kim
  • Function : Author
Seung-Lee Kim
  • Function : Author
Chung-Uk Lee
  • Function : Author
Dong-Joo Lee
  • Function : Author
Yongseok Lee
  • Function : Author
Byeong-Gon Park
  • Function : Author
Richard W. Pogge
  • Function : Author
Matthew T. Penny
  • Function : Author
Shude Mao
  • Function : Author
Tianshu Wang
  • Function : Author

Abstract

We report the discovery of a low-mass-ratio planet (q = 1.3 × 10-4), i.e., 2.5 times higher than the Neptune/Sun ratio. The planetary system was discovered from the analysis of the KMT-2017-BLG-0165 microlensing event, which has an obvious short-term deviation from the underlying light curve produced by the host of the planet. Although the fit improvement with the microlens parallax effect is relatively low, one component of the parallax vector is strongly constrained from the light curve, making it possible to narrow down the uncertainties of the lens physical properties. A Bayesian analysis yields that the planet has a super-Neptune mass ({M}2={34}-12+15 {M}\oplus ) orbiting a Sun-like star ({M}1={0.76}-0.27+0.34 {M}) located at 4.5 kpc. The blended light is consistent with these host properties. The projected planet-host separation is {a}\perp ={3.45}-0.95+0.98 {au}, implying that the planet is located outside the snow line of the host, i.e., a sl ∼ 2.1 au. KMT-2017-BLG-0165Lb is the sixteenth microlensing planet with mass ratio q < 3 × 10-4. Using the fifteen of these planets with unambiguous mass-ratio measurements, we apply a likelihood analysis to investigate the form of the mass-ratio function in this regime. If we adopt a broken power law for the form of this function, then the break is at q br ≃ 0.55 × 10-4, which is much lower than previously estimated. Moreover, the change of the power-law slope, ζ > 3.3, is quite severe. Alternatively, the distribution is also suggestive of a pileup of planets at Neptune-like mass ratios, below which there is a dramatic drop in frequency.

Dates and versions

insu-03674464 , version 1 (20-05-2022)

Identifiers

Cite

Youn Kil Jung, Andrew Gould, Weicheng Zang, Kyu-Ha Hwang, Yoon-Hyun Ryu, et al.. KMT-2017-BLG-0165Lb: A Super-Neptune-mass Planet Orbiting a Sun-like Host Star. The Astronomical Journal, 2019, 157, ⟨10.3847/1538-3881/aaf87f⟩. ⟨insu-03674464⟩
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