Chemical and Isotopic Homogeneity between the L Dwarf CD-35 2722 B and Its Early M Host Star

Abstract CD-35 2722 B is an L dwarf companion to the nearby, ∼50–200 Myr old M1 dwarf CD-35 2722 A. We present a detailed analysis of both objects using high-resolution ( R ∼ 35,000) K -band spectroscopy from the Keck Planet Imager and Characterizer combined with archival photometry. With a mass of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mn>3</mml:mn> <mml:msubsup> <mml:mrow> <mml:mn>0</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>4</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>5</mml:mn> </mml:mrow> </mml:msubsup> <mml:mspace width="1em"/> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">Jup</mml:mi> </mml:mrow> </mml:msub> </mml:math> (planet-to-host mass ratio 0.05) and projected separation of 67 ± 4 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 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo stretchy="false">[</mml:mo> <mml:mi mathvariant="normal">M</mml:mi> <mml:mo>/</mml:mo> <mml:mi mathvariant="normal">H</mml:mi> <mml:mo stretchy="false">]</mml:mo> <mml:mo>=</mml:mo> <mml:mo>−</mml:mo> <mml:mn>0</mml:mn> <mml:mo>.</mml:mo> <mml:msubsup> <mml:mn>16</mml:mn> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0</mml:mn> <mml:mo>.</mml:mo> <mml:mn>02</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0</mml:mn> <mml:mo>.</mml:mo> <mml:mn>03</mml:mn> </mml:mrow> </mml:msubsup> <mml:mspace width="0.25em"/> <mml:mo stretchy="false">(</mml:mo> <mml:mi>stat</mml:mi> <mml:mo stretchy="false">)</mml:mo> <mml:mo>±</mml:mo> <mml:mn>0</mml:mn> <mml:mo>.</mml:mo> <mml:mn>25</mml:mn> <mml:mspace width="0.25em"/> <mml:mo stretchy="false">(</mml:mo> <mml:mi>sys</mml:mi> <mml:mo stretchy="false">)</mml:mo> </mml:math> dex and <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msup> <mml:mrow/> <mml:mrow> <mml:mn>12</mml:mn> </mml:mrow> </mml:msup> <mml:mi mathvariant="normal">C</mml:mi> <mml:msup> <mml:mrow> <mml:mo>/</mml:mo> </mml:mrow> <mml:mrow> <mml:mn>13</mml:mn> </mml:mrow> </mml:msup> <mml:mi mathvariant="normal">C</mml:mi> <mml:mspace width="0.214em"/> <mml:mo>=</mml:mo> <mml:mn>13</mml:mn> <mml:msubsup> <mml:mrow> <mml:mn>2</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>14</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>20</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> for the host, and <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo stretchy="false">[</mml:mo> <mml:mi mathvariant="normal">M</mml:mi> <mml:mo>/</mml:mo> <mml:mi mathvariant="normal">H</mml:mi> <mml:mo stretchy="false">]</mml:mo> <mml:mo>=</mml:mo> <mml:mn>0</mml:mn> <mml:mo>.</mml:mo> <mml:msubsup> <mml:mn>27</mml:mn> <mml:mi>-0.06</mml:mi> <mml:mi>+0.07</mml:mi> </mml:msubsup> <mml:mspace width="0.25em"/> <mml:mo stretchy="false">(</mml:mo> <mml:mi>stat</mml:mi> <mml:mo stretchy="false">)</mml:mo> <mml:mi>±0.12</mml:mi> <mml:mspace width="0.25em"/> <mml:mo stretchy="false">(</mml:mo> <mml:mi>sys</mml:mi> <mml:mo stretchy="false">)</mml:mo> </mml:math> dex, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msup> <mml:mrow/> <mml:mn>12</mml:mn> </mml:msup> <mml:mi>CO</mml:mi> <mml:msup> <mml:mo>/</mml:mo> <mml:mn>13</mml:mn> </mml:msup> <mml:mi>CO</mml:mi> <mml:mo>=</mml:mo> <mml:msubsup> <mml:mn>159</mml:mn> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>24</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>33</mml:mn> </mml:mrow> </mml:msubsup> <mml:mspace width="0.25em"/> <mml:msubsup> <mml:mrow> <mml:mo stretchy="false">(</mml:mo> <mml:mi>stat</mml:mi> <mml:mo stretchy="false">)</mml:mo> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>33</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>40</mml:mn> </mml:mrow> </mml:msubsup> <mml:mspace width="0.25em"/> <mml:mo stretchy="false">(</mml:mo> <mml:mi>sys</mml:mi> <mml:mo stretchy="false">)</mml:mo> </mml:math> , and C/O = 0.55 ± 0.01 (stat) ± 0.04 (sys) for the companion. The chemical compositions for the brown dwarf and host star agree within the 1.5 σ 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 str

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Publication Details

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The Astrophysical Journal
Published
2026-01-22
DOI
https://doi.org/10.3847/1538-4357/ae232f
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2
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Stellar, planetary, and galactic studies
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article
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article

Chemical and Isotopic Homogeneity between the L Dwarf CD-35 2722 B and Its Early M Host Star

Caprice L. Phillips, Randall Bartos, D. González Picos, Chih-Chun Hsu et al.
2 citations
The Astrophysical Journal
Stellar, planetary, and galactic studies
47.65
article

Chemical and Isotopic Homogeneity between the L Dwarf CD-35 2722 B and Its Early M Host Star

Caprice L. Phillips, Randall Bartos, D. González Picos, Chih-Chun Hsu, Benjamin Calvin, Yinzi Xin, Jason J. Wang, Jacklyn Pezzato-Rovner, Jerry W. Xuan, Gregory Doppmann, Ji 吉 Wang 王, Ashley Baker, Tobias Schofield, Ben Sappey, Ronald Orozco López, Jean-Baptiste Ruffio, Geoffrey A. Blake, Sylvain Cetre, Jacques-Robert Delorme, Evan Morris, Nemanja Jovanovic, Dimitri Mawet, Katelyn Horstman, Yapeng Zhang, Joshua Liberman, Daniel Echeverri, Luke Finnerty, Zhoujian 周健 Zhang 张, Andrew Skemer, Michael P. Fitzgerald, J. Kent Wallace, Gavin Wang
article en
2 citations

Abstract

Abstract CD-35 2722 B is an L dwarf companion to the nearby, ∼50–200 Myr old M1 dwarf CD-35 2722 A. We present a detailed analysis of both objects using high-resolution ( R ∼ 35,000) K -band spectroscopy from the Keck Planet Imager and Characterizer combined with archival photometry. With a mass of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mn>3</mml:mn> <mml:msubsup> <mml:mrow> <mml:mn>0</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>4</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>5</mml:mn> </mml:mrow> </mml:msubsup> <mml:mspace width="1em"/> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">Jup</mml:mi> </mml:mrow> </mml:msub> </mml:math> (planet-to-host mass ratio 0.05) and projected separation of 67 ± 4 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 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo stretchy="false">[</mml:mo> <mml:mi mathvariant="normal">M</mml:mi> <mml:mo>/</mml:mo> <mml:mi mathvariant="normal">H</mml:mi> <mml:mo stretchy="false">]</mml:mo> <mml:mo>=</mml:mo> <mml:mo>−</mml:mo> <mml:mn>0</mml:mn> <mml:mo>.</mml:mo> <mml:msubsup> <mml:mn>16</mml:mn> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0</mml:mn> <mml:mo>.</mml:mo> <mml:mn>02</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0</mml:mn> <mml:mo>.</mml:mo> <mml:mn>03</mml:mn> </mml:mrow> </mml:msubsup> <mml:mspace width="0.25em"/> <mml:mo stretchy="false">(</mml:mo> <mml:mi>stat</mml:mi> <mml:mo stretchy="false">)</mml:mo> <mml:mo>±</mml:mo> <mml:mn>0</mml:mn> <mml:mo>.</mml:mo> <mml:mn>25</mml:mn> <mml:mspace width="0.25em"/> <mml:mo stretchy="false">(</mml:mo> <mml:mi>sys</mml:mi> <mml:mo stretchy="false">)</mml:mo> </mml:math> dex and <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msup> <mml:mrow/> <mml:mrow> <mml:mn>12</mml:mn> </mml:mrow> </mml:msup> <mml:mi mathvariant="normal">C</mml:mi> <mml:msup> <mml:mrow> <mml:mo>/</mml:mo> </mml:mrow> <mml:mrow> <mml:mn>13</mml:mn> </mml:mrow> </mml:msup> <mml:mi mathvariant="normal">C</mml:mi> <mml:mspace width="0.214em"/> <mml:mo>=</mml:mo> <mml:mn>13</mml:mn> <mml:msubsup> <mml:mrow> <mml:mn>2</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>14</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>20</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> for the host, and <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo stretchy="false">[</mml:mo> <mml:mi mathvariant="normal">M</mml:mi> <mml:mo>/</mml:mo> <mml:mi mathvariant="normal">H</mml:mi> <mml:mo stretchy="false">]</mml:mo> <mml:mo>=</mml:mo> <mml:mn>0</mml:mn> <mml:mo>.</mml:mo> <mml:msubsup> <mml:mn>27</mml:mn> <mml:mi>-0.06</mml:mi> <mml:mi>+0.07</mml:mi> </mml:msubsup> <mml:mspace width="0.25em"/> <mml:mo stretchy="false">(</mml:mo> <mml:mi>stat</mml:mi> <mml:mo stretchy="false">)</mml:mo> <mml:mi>±0.12</mml:mi> <mml:mspace width="0.25em"/> <mml:mo stretchy="false">(</mml:mo> <mml:mi>sys</mml:mi> <mml:mo stretchy="false">)</mml:mo> </mml:math> dex, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msup> <mml:mrow/> <mml:mn>12</mml:mn> </mml:msup> <mml:mi>CO</mml:mi> <mml:msup> <mml:mo>/</mml:mo> <mml:mn>13</mml:mn> </mml:msup> <mml:mi>CO</mml:mi> <mml:mo>=</mml:mo> <mml:msubsup> <mml:mn>159</mml:mn> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>24</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>33</mml:mn> </mml:mrow> </mml:msubsup> <mml:mspace width="0.25em"/> <mml:msubsup> <mml:mrow> <mml:mo stretchy="false">(</mml:mo> <mml:mi>stat</mml:mi> <mml:mo stretchy="false">)</mml:mo> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>33</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>40</mml:mn> </mml:mrow> </mml:msubsup> <mml:mspace width="0.25em"/> <mml:mo stretchy="false">(</mml:mo> <mml:mi>sys</mml:mi> <mml:mo stretchy="false">)</mml:mo> </mml:math> , and C/O = 0.55 ± 0.01 (stat) ± 0.04 (sys) for the companion. The chemical compositions for the brown dwarf and host star agree within the 1.5 σ 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 str

The Astrophysical JournalVol. 997(2)
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