학술논문
The mass determination of TOI-519 b: a close-in giant planet transiting a metal-rich mid-M dwarf
Document Type
Working Paper
Author
Kagetani, Taiki; Narita, Norio; Kimura, Tadahiro; Hirano, Teruyuki; Ikoma, Masahiro; Ishikawa, Hiroyuki Tako; Giacalone, Steven; Fukui, Akihiko; Kodama, Takanori; Gore, Rebecca; Schroeder, Ashley; Hori, Yasunori; Kawauchi, Kiyoe; Watanabe, Noriharu; Mori, Mayuko; Zou, Yujie; Ikuta, Kai; Krishnamurthy, Vigneshwaran; Zink, Jon; Hardegree-Ullman, Kevin; Harakawa, Hiroki; Kudo, Tomoyuki; Kotani, Takayuki; Kurokawa, Takashi; Kusakabe, Nobuhiko; Kuzuhara, Masayuki; de Leon, Jerome P.; Livingston, John H.; Nishikawa, Jun; Omiya, Masashi; Palle, Enric; Parviainen, Hannu; Serizawa, Takuma; Teng, Huan-Yu; Ueda, Akitoshi; Tamura, Motohide
Source
Subject
Language
Abstract
We report the mass determination of TOI-519 b, a transiting substellar object around a mid-M dwarf. We carried out radial velocity measurements using Subaru / InfraRed Doppler (IRD), revealing that TOI-519 b is a planet with a mass of $0.463^{+0.082}_{-0.088}~M_{\rm Jup}$. We also find that the host star is metal rich ($\rm [Fe/H] = 0.27 \pm 0.09$ dex) and has the lowest effective temperature ($T_{\rm eff}=3322 \pm 49$ K) among all stars hosting known close-in giant planets based on the IRD spectra and mid-resolution infrared spectra obtained with NASA Infrared Telescope Facility / SpeX. The core mass of TOI-519 b inferred from a thermal evolution model ranges from $0$ to $\sim30~M_\oplus$, which can be explained by both the core accretion and disk instability models as the formation origins of this planet. However, TOI-519 is in line with the emerging trend that M dwarfs with close-in giant planets tend to have high metallicity, which may indicate that they formed in the core accretion model. The system is also consistent with the potential trend that close-in giant planets around M dwarfs tend to be less massive than those around FGK dwarfs.
Comment: 10 pages, 5 figures. Accepted for publication in PASJ
Comment: 10 pages, 5 figures. Accepted for publication in PASJ