Rotation and Abundances of the Benchmark Brown Dwarf HD 33632 Ab from Keck/KPIC High-resolution Spectroscopy
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| Format: | Preprint |
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2024
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| author | Hsu, Chih-Chun Wang, Jason J. Xuan, Jerry W. Ruffio, Jean-Baptiste Echeverri, Daniel Xin, Yinzi Liberman, Joshua Finnerty, Luke Morris, Evan Horstman, Katelyn Sappey, Ben Doppmann, Gregory W. Mawet, Dimitri Jovanovic, Nemanja Fitzgerald, Michael P. Delorme, Jacques-Robert Wallace, J. Kent Baker, Ashley Bartos, Randall Blake, Geoffrey A. Calvin, Benjamin Cetre, Sylvain López, Ronald A. Pezzato, Jacklyn Schofield, Tobias Skemer, Andrew Wang, Ji |
| author_facet | Hsu, Chih-Chun Wang, Jason J. Xuan, Jerry W. Ruffio, Jean-Baptiste Echeverri, Daniel Xin, Yinzi Liberman, Joshua Finnerty, Luke Morris, Evan Horstman, Katelyn Sappey, Ben Doppmann, Gregory W. Mawet, Dimitri Jovanovic, Nemanja Fitzgerald, Michael P. Delorme, Jacques-Robert Wallace, J. Kent Baker, Ashley Bartos, Randall Blake, Geoffrey A. Calvin, Benjamin Cetre, Sylvain López, Ronald A. Pezzato, Jacklyn Schofield, Tobias Skemer, Andrew Wang, Ji |
| contents | We present the projected rotational velocity and molecular abundances for HD 33632 Ab obtained via Keck Planet Imager and Characterizer high-resolution spectroscopy. HD 33632 Ab is a nearby benchmark brown dwarf companion at a separation of $\sim$20 au that straddles the L/T transition. Using a forward-modeling framework with on-axis host star spectra, self-consistent substellar atmospheric and retrieval models for HD 33632 Ab, we derive a projected rotational velocity of 53 $\pm$ 3 km/s and carbon/water mass fractions of log CO = $-$2.3 $\pm$ 0.3 and log H$_2$O = $-$2.7 $\pm$ 0.2. The inferred carbon-to-oxygen ratio (C/O = 0.58 $\pm$ 0.14), molecular abundances, and metallicity ([C/H] = 0.0 $\pm$ 0.2 dex) of HD 33632 Ab are consistent with its host star. Although detectable methane opacities are expected in L/T transition objects, we did not recover methane in our KPIC spectra, partly due to the high $v\sin{i}$ and to disequilibrium chemistry at the pressures we are sensitive to. We parameterize the spin as the ratio of rotation over break-up velocity, and compare HD 33632 Ab to a compilation of >200 very low-mass objects (M$\lesssim$0.1 M$_{\odot}$) that have spin measurements in the literature. There appears to be no clear trend for the isolated field low-mass objects versus mass, but a tentative trend is identified for low-mass companions and directly imaged exoplanets, similar to previous findings. A larger sample of close-in gas giant exoplanets and brown dwarfs will critically examine our understanding of their formation and evolution through rotation and chemical abundance measurements. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2405_08312 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Rotation and Abundances of the Benchmark Brown Dwarf HD 33632 Ab from Keck/KPIC High-resolution Spectroscopy Hsu, Chih-Chun Wang, Jason J. Xuan, Jerry W. Ruffio, Jean-Baptiste Echeverri, Daniel Xin, Yinzi Liberman, Joshua Finnerty, Luke Morris, Evan Horstman, Katelyn Sappey, Ben Doppmann, Gregory W. Mawet, Dimitri Jovanovic, Nemanja Fitzgerald, Michael P. Delorme, Jacques-Robert Wallace, J. Kent Baker, Ashley Bartos, Randall Blake, Geoffrey A. Calvin, Benjamin Cetre, Sylvain López, Ronald A. Pezzato, Jacklyn Schofield, Tobias Skemer, Andrew Wang, Ji Solar and Stellar Astrophysics Earth and Planetary Astrophysics We present the projected rotational velocity and molecular abundances for HD 33632 Ab obtained via Keck Planet Imager and Characterizer high-resolution spectroscopy. HD 33632 Ab is a nearby benchmark brown dwarf companion at a separation of $\sim$20 au that straddles the L/T transition. Using a forward-modeling framework with on-axis host star spectra, self-consistent substellar atmospheric and retrieval models for HD 33632 Ab, we derive a projected rotational velocity of 53 $\pm$ 3 km/s and carbon/water mass fractions of log CO = $-$2.3 $\pm$ 0.3 and log H$_2$O = $-$2.7 $\pm$ 0.2. The inferred carbon-to-oxygen ratio (C/O = 0.58 $\pm$ 0.14), molecular abundances, and metallicity ([C/H] = 0.0 $\pm$ 0.2 dex) of HD 33632 Ab are consistent with its host star. Although detectable methane opacities are expected in L/T transition objects, we did not recover methane in our KPIC spectra, partly due to the high $v\sin{i}$ and to disequilibrium chemistry at the pressures we are sensitive to. We parameterize the spin as the ratio of rotation over break-up velocity, and compare HD 33632 Ab to a compilation of >200 very low-mass objects (M$\lesssim$0.1 M$_{\odot}$) that have spin measurements in the literature. There appears to be no clear trend for the isolated field low-mass objects versus mass, but a tentative trend is identified for low-mass companions and directly imaged exoplanets, similar to previous findings. A larger sample of close-in gas giant exoplanets and brown dwarfs will critically examine our understanding of their formation and evolution through rotation and chemical abundance measurements. |
| title | Rotation and Abundances of the Benchmark Brown Dwarf HD 33632 Ab from Keck/KPIC High-resolution Spectroscopy |
| topic | Solar and Stellar Astrophysics Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2405.08312 |