Brown Dwarfs

Fresh View Of The Hot Brown Dwarf HD 984 B Through High-resolution Spectroscopy

By Keith Cowing

Press Release

April 20, 2024

Filed under atmosphere, brown dwarf, exoplanet, high-resolution spectroscopy, Keck Planet Imager and Characterizer, petitRADTRANS, Spectroscopy

Fresh View Of The Hot Brown Dwarf HD 984 B Through High-resolution Spectroscopy — The P − T profile from our best-fit retrieval (model MgSiO3 + Fe). The best-fit profile is shown in black, and 200 random draws from the posterior are shown in blue. The condensation curves for different cloud species (MgSiO3, Fe and Al2O3) are also plotted. In addition, we show multiple Sonora P − T profiles as dashed lines (Marley et al. 2021) with similar properties as HD 984 B. Finally, we plot the emission contribution function (in wavelength, top axis) as contours, which quantifies the relative importance of the emission in a given pressure layer to the total at a given wavelength (Mollière et al. 2019). — astro-ph.SR

Context. High-resolution spectroscopy has the potential to drive a better understanding of the atmospheric composition, physics, and dynamics of young exoplanets and brown dwarfs, bringing clear insights into the formation channel of individual objects.

Aims. Using the Keck Planet Imager and Characterizer (KPIC; R = 35,000), we aim to characterize a young brown dwarf HD 984 B. By measuring its C/O and ¹²CO/¹³CO ratios, we expect to gain new knowledge about its origin by confirming the difference in the formation pathways between brown dwarfs and super-Jupiters.

Methods. We analysed the KPIC high-resolution spectrum (2.29-2.49 µm)) of HD 984 B using an atmospheric retrieval framework based on nested sampling and petitRADTRANS, using both clear and cloudy models.

Results. Using our best-fit model, we find C/O = 0.50+0.01-0.01 (0.01 is the statistical error) for HD 984 B which agrees with that of its host star within 1σ (0.40+0.20-0.20). We also retrieve an isotopolog ¹²CO/¹³CO ratio of 98+20-25 in its atmosphere, which is similar to that of the Sun. In addition, HD 984 B has a substellar metallicity with [Fe/H] = -0.62+0.02-0.02. Finally, we find that most of the retrieved parameters are independent of our choice of retrieval model.

Conclusions. From our measured C/O and ¹²CO/¹³CO, the favored formation mechanism of HD 984 B seems to be via gravitational collapse or disk instability and not core accretion, which is a favored formation mechanism for giant exoplanets with m < 13 M_Jup and semimajor axis between 10 and 100 au. However, with only a few brown dwarfs with a measured ¹²CO/¹³CO ratio, similar analyses using high-resolution spectroscopy will become essential in order to determine planet formation processes more precisely.

J. C. Costes, J. W. Xuan, A. Vigan, J. Wang, V. D’Orazi, P. Mollière, A. Baker, R. Bartos, G. A. Blake, B. Calvin, S. Cetre, J. Delorme, G. Doppmann, D. Echeveri, L. Finnerty, M. P. Fitzgerald, C. Hsu, N. Jovanovic, R. Lopez, D. Mawet, E. Morris, J. Pezzato, C. L. Phillips, J. Ruffio, B. Sappey, A. Schneeberger, T. Schofield, A. J. Skemer, J. K. Wallace, J. Wang

Comments: 14 pages, 8 figures
Subjects: Solar and Stellar Astrophysics (astro-ph.SR); Earth and Planetary Astrophysics (astro-ph.EP)
Cite as: arXiv:2404.11523 [astro-ph.SR] (or arXiv:2404.11523v1 [astro-ph.SR] for this version)
Submission history
From: Jean Costes
[v1] Wed, 17 Apr 2024 16:15:23 UTC (8,881 KB)
https://arxiv.org/abs/2404 .11523

Astrobiology

Keith Cowing

Explorers Club Fellow, ex-NASA Space Station Payload manager/space biologist, Away Teams, Journalist, Lapsed climber, Synaesthete, Na’Vi-Jedi-Freman-Buddhist-mix, ASL, Devon Island and Everest Base Camp veteran, (he/him) 🖖🏻

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