Orbital and Atmospheric Characterization of the 1RXS J034231.8+121622 System using High-resolution Spectroscopy Confirms that the Companion is a Low-mass Star
- Creators
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Do Ó, Clarissa R.
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Sappey, Ben
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Konopacky, Quinn M.
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Ruffio, Jean-Baptiste
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O'Neil, Kelly K.
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Do, Tuan
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Martinez, Gregory
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Barman, Travis S.
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Nguyen, Jayke S.
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Xuan, Jerry W.1
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Theissen, Christopher A.
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Blunt, Sarah
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Thompson, William
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Hsu, Chih-Chun
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Baker, Ashley
- Bartos, Randall
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Blake, Geoffrey A.1
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Calvin, Benjamin
- Cetre, Sylvain
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Delorme, Jacques-Robert
- Doppmann, Greg
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Echeverri, Daniel
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Finnerty, Luke
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Fitzgerald, Michael P.
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Inglis, Julie
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Jovanovic, Nemanja1
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López, Ronald A.
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Mawet, Dimitri1
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Morris, Evan
- Pezzato, Jacklyn
- Schofield, Tobias
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Skemer, Andrew
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Wallace, J. Kent
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Wang, Jason J.1
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Wang, Ji
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Liberman, Joshua
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1.
California Institute of Technology
Abstract
The 1RXS J034231.8+121622 system consists of an M dwarf primary and a directly imaged low-mass stellar companion. We use high-resolution spectroscopic data from Keck/KPIC to estimate the objects' atmospheric parameters and radial velocities (RVs). Using PHOENIX stellar models, we find that the primary has a temperature of 3460 ± 50 K and a metallicity of 0.16 ± 0.04, while the secondary has a temperature of 2510 ± 50 K and a metallicity of 0.13_(−0.11)^(+0.12). Recent work suggests this system is associated with the Hyades, giving it an older age than previous estimates. Both metallicities agree with current Hyades [Fe/H] measurements (0.11–0.21). Using stellar evolutionary models, we obtain significantly higher masses for the objects, 0.30 ± 0.15 M⊙ and 0.08 ± 0.01 M⊙ (84 ± 11 MJup), respectively. Using the RVs and a new astrometry point from Keck/NIRC2, we find that the system is likely an edge-on, moderately eccentric (0.41_(−0.08)^(+0.27)) configuration. We also estimate the C/O ratio of both objects using custom grid models, obtaining 0.42 ± 0.10 (primary) and 0.55 ± 0.10 (companion). From these results, we confirm that this system most likely went through a binary star formation process in the Hyades. The significant changes in this system's parameters since its discovery highlight the importance of high-resolution spectroscopy for both orbital and atmospheric characterization of directly imaged companions.
Copyright and License
© 2024. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.
Acknowledgement
We thankfully acknowledge Brendan Bowler for sharing OSIRIS data on 1RXS J034231.8+121622. We also thank the anonymous referee for providing comments that helped improve this manuscript.
Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The W. M. Keck Observatory was made possible by the financial support of the W. M. Keck Foundation. The authors wish to acknowledge the significant cultural role that the summit of Maunakea has always had within the indigenous Hawaiian community. The authors are extremely fortunate to conduct observations from this mountain. Portions of this work were conducted at the University of California, San Diego, which was built on the unceded territory of the Kumeyaay Nation, whose people continue to maintain their political sovereignty and cultural traditions as vital members of the San Diego community.
C.D.O. is supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE-2038238. Further support for this work at UCLA was provided by the W. M. Keck Foundation, and NSF Grant No. AST-1909554. J.X. acknowledges support from the NASA Future Investigators in NASA Earth and Space Science and Technology (FINESST) award #80NSSC23K1434. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation.
Funding for KPIC has been provided by the California Institute of Technology, the Jet Propulsion Laboratory, the Heising-Simons Foundation (grants #2015-129, #2017-318, #2019-1312, and #2023-4598), the Simons Foundation (through the Caltech Center for Comparative Planetary Evolution), and the NSF under grant No. AST-1611623.
Part of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA (80NM00018D0004).
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Additional details
- ISSN
- 1538-3881
- W. M. Keck Foundation
- National Science Foundation
- NSF Graduate Research Fellowship DGE-2038238
- National Aeronautics and Space Administration
- NASA Earth and Space Science and Technology Fellowship027ka1x80 80NSSC23K1434
- California Institute of Technology
- Jet Propulsion Laboratory
- Heising-Simons Foundation
- 2015-129
- Heising-Simons Foundation
- 2017-318
- Heising-Simons Foundation
- 2019-1312
- Heising-Simons Foundation
- 2023-4598
- Simons Foundation
- National Science Foundation
- AST-1611623
- National Aeronautics and Space Administration
- 80NM00018D0004
- Caltech groups
- Astronomy Department, Division of Geological and Planetary Sciences, Caltech Center for Comparative Planetary Evolution