The Astronomical Journal (Jan 2025)

HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer

  • Ben Sappey,
  • Quinn Konopacky,
  • Clarissa R. Do Ó,
  • Travis Barman,
  • Jean-Baptiste Ruffio,
  • Jason Wang,
  • Christopher A. Theissen,
  • Luke Finnerty,
  • Jerry Xuan,
  • Katelyn Hortsman,
  • Dimitri Mawet,
  • Yapeng Zhang,
  • Julie Inglis,
  • Nicole L. Wallack,
  • Aniket Sanghi,
  • Ashley Baker,
  • Randall Bartos,
  • Geoffrey A. Blake,
  • Charlotte Z. Bond,
  • Benjamin Calvin,
  • Sylvain Cetre,
  • Jacques-Robert Delorme,
  • Greg Doppmann,
  • Daniel Echeverri,
  • Michael P. Fitzgerald,
  • Chih-Chun Hsu,
  • Nemanja Jovanovic,
  • Joshua Liberman,
  • Ronald A. López,
  • Emily C. Martin,
  • Evan Morris,
  • Jacklyn Pezzato-Rovner,
  • Caprice L. Phillips,
  • Garreth Ruane,
  • Tobias Schofield,
  • Andrew Skemer,
  • Taylor Venenciano,
  • J. Kent Wallace,
  • Ji Wang,
  • Peter Wizinowich,
  • Yinzi Xin

DOI
https://doi.org/10.3847/1538-3881/adad70
Journal volume & issue
Vol. 169, no. 3
p. 175

Abstract

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We present an atmospheric characterization and orbital analysis of HD 206893 B, an exceptionally red, L/T-transition substellar companion in a multiplanetary system, via Keck Planet Imager and Characterizer (KPIC) high-resolution ( R ∼ 35,000) K- band spectroscopy. Using PHOENIX atmospheric models in a forward-model framework that fits the spectrum of the companion and diffracted starlight simultaneously, we detect HD 206893 B at >8 σ significance via cross correlation in two epochs. We find an effective temperature for the companion of 1634 ${}_{-38}^{+72}$ K and a $\mathrm{log}\,g$ of 4.55 ${}_{-0.22}^{+0.17}$ . Only accounting for statistical uncertainties, we measure the carbon-oxygen ratio (C/O) of this companion to be 0.57 ± 0.02, or near-solar while assuming solar metallicity. The C/O ratio we measure fits the tentative trend of >4 M _Jup companions having near-solar C/O ratios while less massive companions have greater-than-solar C/O ratios. Using substellar evolution models, we find an age of 112 ${}_{-22}^{+36}$ Myr, a mass of 22.7 ${}_{-1.7}^{+2.5}$ M _Jup , and a radius of 1.11 ± 0.03 R _Jup for this companion. We also use KPIC radial velocity data to fit the orbit of HD 206893 B and analyze the orbital stability of this system. We find that the orbital stability is relatively independent of the mass of HD 206893 B, and favors an orbital configuration where B and its interior planetary companion, HD 206893 c, are coplanar. The measured C/O ratio coupled with the current architecture of the system cannot rule out the core accretion scenario, nor the disk fragmentation scenario regarding the formation pathway of HD 206893 B.

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