The Astronomical Journal (Jan 2022)

Retrieving C and O Abundance of HR 8799 c by Combining High- and Low-resolution Data

  • Ji Wang,
  • Jason J. Wang,
  • Jean-Baptiste Ruffio,
  • Geoffrey A. Blake,
  • Dimitri Mawet,
  • Ashley Baker,
  • Randall Bartos,
  • Charlotte Z. Bond,
  • Benjamin Calvin,
  • Sylvain Cetre,
  • Jacques-Robert Delorme,
  • Greg Doppmann,
  • Daniel Echeverri,
  • Luke Finnerty,
  • Michael P. Fitzgerald,
  • Nemanja Jovanovic,
  • Ronald Lopez,
  • Emily C. Martin,
  • Evan Morris,
  • Jacklyn Pezzato,
  • Sam Ragland,
  • Garreth Ruane,
  • Ben Sappey,
  • Tobias Schofield,
  • Andrew Skemer,
  • Taylor Venenciano,
  • J. Kent Wallace,
  • Peter Wizinowich,
  • Jerry W. Xuan,
  • Marta L. Bryan,
  • Arpita Roy,
  • Nicole L. Wallack

DOI
https://doi.org/10.3847/1538-3881/ac9f19
Journal volume & issue
Vol. 165, no. 1
p. 4

Abstract

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The formation and evolution pathway for the directly imaged multiplanetary system HR 8799 remains mysterious. Accurate constraints on the chemical composition of the planetary atmosphere(s) are key to solving the mystery. We perform a detailed atmospheric retrieval on HR 8799 c to infer the chemical abundances and abundance ratios using a combination of photometric data along with low- and high-resolution spectroscopic data ( R ∼ 20–35,000). We specifically retrieve [C/H], [O/H], and C/O and find them to be ${0.55}_{-0.39}^{+0.36}$ , ${0.47}_{-0.32}^{+0.31}$ , and ${0.67}_{-0.15}^{+0.12}$ at 68% confidence. The superstellar C and O abundances, yet a stellar C/O ratio, reveal a potential formation pathway for HR 8799 c. Planet c, and likely the other gas giant planets in the system, formed early on (likely within ∼1 Myr), followed by further atmospheric enrichment in C and O through the accretion of solids beyond the CO ice line. The enrichment either preceded or took place during the early phase of the inward migration to the current planet locations.

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