KMT-2017-BLG-0165Lb: A Super-Neptune-mass Planet Orbiting a Sun-like Host Star - INSU - Institut national des sciences de l'Univers Accéder directement au contenu
Article Dans Une Revue The Astronomical Journal Année : 2019

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

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

Résumé

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 et versions

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

Identifiants

Citer

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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