The Astronomical Journal (Jan 2023)

A Mini-Neptune Orbiting the Metal-poor K Dwarf BD+29 2654

  • Fei Dai,
  • Kevin C. Schlaufman,
  • Henrique Reggiani,
  • Luke Bouma,
  • Andrew W. Howard,
  • Ashley Chontos,
  • Daria Pidhorodetska,
  • Judah Van Zandt,
  • Joseph M. Akana Murphy,
  • Ryan A. Rubenzahl,
  • Alex S. Polanski,
  • Jack Lubin,
  • Corey Beard,
  • Steven Giacalone,
  • Rae Holcomb,
  • Natalie M. Batalha,
  • Ian Crossfield,
  • Courtney Dressing,
  • Benjamin Fulton,
  • Daniel Huber,
  • Howard Isaacson,
  • Stephen R. Kane,
  • Erik A. Petigura,
  • Paul Robertson,
  • Lauren M. Weiss,
  • Alexander A. Belinski,
  • Andrew W. Boyle,
  • Christopher J. Burke,
  • Amadeo Castro-González,
  • David R. Ciardi,
  • Tansu Daylan,
  • Akihiko Fukui,
  • Holden Gill,
  • Natalia M. Guerrero,
  • Coel Hellier,
  • Steve B. Howell,
  • Jorge Lillo-Box,
  • Felipe Murgas,
  • Norio Narita,
  • Enric Pallé,
  • David R. Rodriguez,
  • Arjun B. Savel,
  • Avi Shporer,
  • Keivan G. Stassun,
  • Stephanie Striegel,
  • Douglas A. Caldwell,
  • Jon M. Jenkins,
  • George R. Ricker,
  • Sara Seager,
  • Roland Vanderspek,
  • Joshua N. Winn

DOI
https://doi.org/10.3847/1538-3881/acdee8
Journal volume & issue
Vol. 166, no. 2
p. 49

Abstract

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We report the discovery and Doppler mass measurement of a 7.4 days 2.3 R _⊕ mini-Neptune around a metal-poor K dwarf BD+29 2654 (TOI-2018). Based on a high-resolution Keck/HIRES spectrum, the Gaia parallax, and multiwavelength photometry from the UV to the mid-infrared, we found that the host star has ${T}_{\mathrm{eff}}={4174}_{-42}^{+34}$ K, $\mathrm{log}g={4.62}_{-0.03}^{+0.02}$ , [Fe/H] = − 0.58 ± 0.18, M _* = 0.57 ± 0.02 M _⊙ , and R _* = 0.62 ± 0.01 R _⊙ . Precise Doppler measurements with Keck/HIRES revealed a planetary mass of M _p = 9.2 ± 2.1 M _⊕ for TOI-2018 b. TOI-2018 b has a mass and radius that are consistent with an Earthlike core, with a ∼1%-by-mass hydrogen/helium envelope or an ice–rock mixture. The mass of TOI-2018 b is close to the threshold for runaway accretion and hence giant planet formation. Such a threshold is predicted to be around 10 M _⊕ or lower for a low-metallicity (low-opacity) environment. If TOI-2018 b is a planetary core that failed to undergo runaway accretion, it may underline the reason why giant planets are rare around low-metallicity host stars (one possibility is their shorter disk lifetimes). With a K -band magnitude of 7.1, TOI-2018 b may be a suitable target for transmission spectroscopy with the James Webb Space Telescope. The system is also amenable to metastable Helium observation; the detection of a Helium exosphere would help distinguish between a H/He-enveloped planet and a water world.

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