The Astrophysical Journal (Jan 2024)

Validation of Elemental and Isotopic Abundances in Late-M Spectral Types with the Benchmark HIP 55507 AB System

  • Jerry W. Xuan,
  • Jason Wang,
  • Luke Finnerty,
  • Katelyn Horstman,
  • Simon Grimm,
  • Anne E. Peck,
  • Eric Nielsen,
  • Heather A. Knutson,
  • Dimitri Mawet,
  • Howard Isaacson,
  • Andrew W. Howard,
  • Michael C. Liu,
  • Sam Walker,
  • Mark W. Phillips,
  • Geoffrey A. Blake,
  • Jean-Baptiste Ruffio,
  • Yapeng Zhang,
  • Julie Inglis,
  • Nicole L. Wallack,
  • Aniket Sanghi,
  • Erica J. Gonzales,
  • Fei Dai,
  • Ashley Baker,
  • Randall Bartos,
  • Charlotte Z. Bond,
  • Marta L. Bryan,
  • Benjamin Calvin,
  • Sylvain Cetre,
  • Jacques-Robert Delorme,
  • Greg Doppmann,
  • Daniel Echeverri,
  • Michael P. Fitzgerald,
  • Nemanja Jovanovic,
  • Joshua Liberman,
  • Ronald A. López,
  • Emily C. Martin,
  • Evan Morris,
  • Jacklyn Pezzato,
  • Garreth Ruane,
  • Ben Sappey,
  • Tobias Schofield,
  • Andrew Skemer,
  • Taylor Venenciano,
  • J. Kent Wallace,
  • Ji Wang,
  • Peter Wizinowich,
  • Yinzi Xin,
  • Shubh Agrawal,
  • Clarissa R. Do Ó,
  • Chih-Chun Hsu,
  • Caprice L. Phillips

DOI
https://doi.org/10.3847/1538-4357/ad1243
Journal volume & issue
Vol. 962, no. 1
p. 10

Abstract

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M dwarfs are common host stars to exoplanets but often lack atmospheric abundance measurements. Late-M dwarfs are also good analogs to the youngest substellar companions, which share similar T _eff ∼ 2300–2800 K. We present atmospheric analyses for the M7.5 companion HIP 55507 B and its K6V primary star with Keck/KPIC high-resolution ( R ∼ 35,000) K -band spectroscopy. First, by including KPIC relative radial velocities between the primary and secondary in the orbit fit, we improve the dynamical mass precision by 60% and find ${M}_{B}={88.0}_{-3.2}^{+3.4}\,{M}_{\mathrm{Jup}}$ , putting HIP 55507 B above the stellar–substellar boundary. We also find that HIP 55507 B orbits its K6V primary star with $a={38}_{-3}^{+4}$ au and e = 0.40 ± 0.04. From atmospheric retrievals of HIP 55507 B, we measure [C/H] = 0.24 ± 0.13, [O/H] = 0.15 ± 0.13, and C/O = 0.67 ± 0.04. Moreover, we strongly detect ^13 CO (7.8 σ significance) and tentatively detect ${{\rm{H}}}_{2}^{18}{\rm{O}}$ (3.7 σ significance) in the companion’s atmosphere and measure ${}^{12}\mathrm{CO}{/}^{13}\mathrm{CO}={98}_{-22}^{+28}$ and ${{\rm{H}}}_{2}^{16}{\rm{O}}/{{\rm{H}}}_{2}^{18}{\rm{O}}={240}_{-80}^{+145}$ after accounting for systematic errors. From a simplified retrieval analysis of HIP 55507 A, we measure ${}^{12}\mathrm{CO}{/}^{13}\mathrm{CO}={79}_{-16}^{+21}$ and ${{\rm{C}}}^{16}{\rm{O}}/{{\rm{C}}}^{18}{\rm{O}}={288}_{-70}^{+125}$ for the primary star. These results demonstrate that HIP 55507 A and B have consistent ^12 C/ ^13 C and ^16 O/ ^18 O to the <1 σ level, as expected for a chemically homogeneous binary system. Given the similar flux ratios and separations between HIP 55507 AB and systems with young substellar companions, our results open the door to systematically measuring ^13 CO and ${{\rm{H}}}_{2}^{18}{\rm{O}}$ abundances in the atmospheres of substellar or even planetary-mass companions with similar spectral types.

Keywords