Chemical and Isotopic Homogeneity Between the L Dwarf CD-35 2722 B and its Early M Host Star
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arXiv
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| Natura: | Preprint |
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2025
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| author | Wang, Gavin Xuan, Jerry Picos, Darío Zhang, Zhoujian Zhang, Yapeng Mawet, Dimitri Hsu, Chih-Chun Wang, Jason Blake, Geoffrey Ruffio, Jean-Baptiste Horstman, Katelyn Sappey, Ben Xin, Yinzi Finnerty, Luke Echeverri, Daniel Jovanovic, Nemanja Baker, Ashley Bartos, Randy Calvin, Benjamin Cetre, Sylvain Delorme, Jacques-Robert Doppmann, Greg Fitzgerald, Michael Liberman, Joshua López, Ronald Morris, Evan Pezzato-Rovner, Jacklyn Phillips, Caprice Schofield, Tobias Skemer, Andrew Wallace, James Wang, Ji |
| author_facet | Wang, Gavin Xuan, Jerry Picos, Darío Zhang, Zhoujian Zhang, Yapeng Mawet, Dimitri Hsu, Chih-Chun Wang, Jason Blake, Geoffrey Ruffio, Jean-Baptiste Horstman, Katelyn Sappey, Ben Xin, Yinzi Finnerty, Luke Echeverri, Daniel Jovanovic, Nemanja Baker, Ashley Bartos, Randy Calvin, Benjamin Cetre, Sylvain Delorme, Jacques-Robert Doppmann, Greg Fitzgerald, Michael Liberman, Joshua López, Ronald Morris, Evan Pezzato-Rovner, Jacklyn Phillips, Caprice Schofield, Tobias Skemer, Andrew Wallace, James Wang, Ji |
| contents | CD-35 2722 B is an L dwarf companion to the nearby, $\sim 50-200$ Myr old M1 dwarf CD-35 2722 A. We present a detailed analysis of both objects using high-resolution ($R \sim 35,000$) $K$ band spectroscopy from the Keck Planet Imager and Characterizer (KPIC) combined with archival photometry. With a mass of $30^{+5}_{-4} M_{\mathrm{Jup}}$ (planet-to-host mass ratio 0.05) and projected separation of $67\pm4$ AU from its host, CD-35 2722 B likely formed via gravitational instability. We explore whether the chemical composition of the system tells a similar story. Accounting for systematic uncertainties, we find $\mathrm{[M/H]}=-0.16^{+0.03}_{-0.02} \mathrm{(stat)} \pm 0.25 \mathrm{(sys)}$ dex and $^{12}\mathrm{C}/^{13}\mathrm{C}=132^{+20}_{-14}$ for the host, and $\mathrm{[M/H]}=0.27^{+0.07}_{-0.06} (\mathrm{stat}) \pm 0.12 (\mathrm{sys})$ dex, $^{12}\mathrm{CO}/^{13}\mathrm{CO}=159^{+33}_{-24} \mathrm{(stat)}^{+40}_{-33} \mathrm{(sys)}$, and $\mathrm{C/O} = 0.55 \pm 0.01 (\mathrm{stat}) \pm 0.04 (\mathrm{sys})$ for the companion. The chemical compositions for the brown dwarf and host star agree within the $1.5σ$ level, supporting a scenario where CD-35 2722 B formed via gravitational instability. We do not find evidence for clouds on CD-35 2722 B despite it being a photometrically red mid-L dwarf and thus expected to be quite cloudy. We retrieve a temperature structure which is more isothermal than models and investigate its impact on our measurements, finding that constraining the temperature structure to self-consistent models does not significantly impact our retrieved chemical properties. Our observations highlight the need for data from complementary wavelength ranges to verify the presence of aerosols in likely cloudy L dwarfs. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2511_19588 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Chemical and Isotopic Homogeneity Between the L Dwarf CD-35 2722 B and its Early M Host Star Wang, Gavin Xuan, Jerry Picos, Darío Zhang, Zhoujian Zhang, Yapeng Mawet, Dimitri Hsu, Chih-Chun Wang, Jason Blake, Geoffrey Ruffio, Jean-Baptiste Horstman, Katelyn Sappey, Ben Xin, Yinzi Finnerty, Luke Echeverri, Daniel Jovanovic, Nemanja Baker, Ashley Bartos, Randy Calvin, Benjamin Cetre, Sylvain Delorme, Jacques-Robert Doppmann, Greg Fitzgerald, Michael Liberman, Joshua López, Ronald Morris, Evan Pezzato-Rovner, Jacklyn Phillips, Caprice Schofield, Tobias Skemer, Andrew Wallace, James Wang, Ji Earth and Planetary Astrophysics Solar and Stellar Astrophysics CD-35 2722 B is an L dwarf companion to the nearby, $\sim 50-200$ Myr old M1 dwarf CD-35 2722 A. We present a detailed analysis of both objects using high-resolution ($R \sim 35,000$) $K$ band spectroscopy from the Keck Planet Imager and Characterizer (KPIC) combined with archival photometry. With a mass of $30^{+5}_{-4} M_{\mathrm{Jup}}$ (planet-to-host mass ratio 0.05) and projected separation of $67\pm4$ AU from its host, CD-35 2722 B likely formed via gravitational instability. We explore whether the chemical composition of the system tells a similar story. Accounting for systematic uncertainties, we find $\mathrm{[M/H]}=-0.16^{+0.03}_{-0.02} \mathrm{(stat)} \pm 0.25 \mathrm{(sys)}$ dex and $^{12}\mathrm{C}/^{13}\mathrm{C}=132^{+20}_{-14}$ for the host, and $\mathrm{[M/H]}=0.27^{+0.07}_{-0.06} (\mathrm{stat}) \pm 0.12 (\mathrm{sys})$ dex, $^{12}\mathrm{CO}/^{13}\mathrm{CO}=159^{+33}_{-24} \mathrm{(stat)}^{+40}_{-33} \mathrm{(sys)}$, and $\mathrm{C/O} = 0.55 \pm 0.01 (\mathrm{stat}) \pm 0.04 (\mathrm{sys})$ for the companion. The chemical compositions for the brown dwarf and host star agree within the $1.5σ$ level, supporting a scenario where CD-35 2722 B formed via gravitational instability. We do not find evidence for clouds on CD-35 2722 B despite it being a photometrically red mid-L dwarf and thus expected to be quite cloudy. We retrieve a temperature structure which is more isothermal than models and investigate its impact on our measurements, finding that constraining the temperature structure to self-consistent models does not significantly impact our retrieved chemical properties. Our observations highlight the need for data from complementary wavelength ranges to verify the presence of aerosols in likely cloudy L dwarfs. |
| title | Chemical and Isotopic Homogeneity Between the L Dwarf CD-35 2722 B and its Early M Host Star |
| topic | Earth and Planetary Astrophysics Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2511.19588 |