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PreprintCC BY 4.0arXiv

Sinking Silicates I: Characterizing the benchmark system containing the T0 brown dwarf CWISE J210640.16+250729.0 using JWST

  • Austin Rothermich
  • Jacqueline K. Faherty
  • Ben Burningham
  • Catherine Manea
  • Emily Calamari
  • Genaro Suárez
  • Daniella C. Bardalez Gagliuffi
  • John M. Brewer
  • Kelle L. Cruz
  • Josefine Gaarn
  • Jonathan Gagné
  • Eileen C. Gonzales
7 more authors
  • Marina E. Gemma
  • Viktória Kecskeméthy
  • Mark S. Marley
  • Caprice L. Phillips
  • Channon Visscher
  • Johanna M. Vos
  • Niall Whiteford
Open at sourcePDFDOICite

Abstract

In this study, we present the full (97.3\% complete) 0.8--12.5 μm spectral energy distribution (SED) of an L/T transition object, CWISE J210640.16+250729.0 (CW2106), using the James Webb Space Telescope (JWST). We provide a full characterization of the host star's elemental abundances and age. We empirically derive the bolometric luminosity (Lbol≈−4.825 textupL⊙) of CW2106, and obtain estimates of its mass (M≈50−62 MJup), radius (R≈0.83−0.87 RJup), effective temperature (Teff≈1213 K), and surface gravity (log g≈5.28 dex). We find the near-infrared (near-IR) spectrum ($0.8-2.5 ~μ$m) is best reproduced with cloudy atmospheric models while the mid-infrared (mid-IR) spectrum ($5-12.5 ~μ$m) is best reproduced with cloudless models. This suggests a cloud layer restricted to only the deepest observable parts of the atmosphere and is qualified by the lack of a 9 μm silicate feature. Making use of the Mg/Si ratio of the primary, alongside thermochemical models, we predict the clouds in CW2106 to be composed primarily of enstatite (MgSiO3), removing ∼23% of the bulk oxygen out of the atmosphere. Future retrieval studies will be able to help investigate the existence and full impact of these cloud species.

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Cite

BibTeXRIS
BibTeX
@misc{rothermich2026sinking,
  title = {{Sinking Silicates I: Characterizing the benchmark system containing the T0 brown dwarf CWISE J210640.16+250729.0 using JWST}},
  author = {Austin Rothermich and Jacqueline K. Faherty and Ben Burningham and Catherine Manea and Emily Calamari and Genaro Suárez and Daniella C. Bardalez Gagliuffi and John M. Brewer and Kelle L. Cruz and Josefine Gaarn and Jonathan Gagné and Eileen C. Gonzales and Marina E. Gemma and Viktória Kecskeméthy and Mark S. Marley and Caprice L. Phillips and Channon Visscher and Johanna M. Vos and Niall Whiteford},
  howpublished = {arXiv},
  year = {2026},
  month = sep,
  doi = {10.48550/arxiv.2609.13433},
  eprint = {2609.13433},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2609.13433},
  note = {CC BY 4.0},
}
RIS
TY  - UNPB
TI  - Sinking Silicates I: Characterizing the benchmark system containing the T0 brown dwarf CWISE J210640.16+250729.0 using JWST
AU  - Austin Rothermich
AU  - Jacqueline K. Faherty
AU  - Ben Burningham
AU  - Catherine Manea
AU  - Emily Calamari
AU  - Genaro Suárez
AU  - Daniella C. Bardalez Gagliuffi
AU  - John M. Brewer
AU  - Kelle L. Cruz
AU  - Josefine Gaarn
AU  - Jonathan Gagné
AU  - Eileen C. Gonzales
AU  - Marina E. Gemma
AU  - Viktória Kecskeméthy
AU  - Mark S. Marley
AU  - Caprice L. Phillips
AU  - Channon Visscher
AU  - Johanna M. Vos
AU  - Niall Whiteford
PY  - 2026
DA  - 2026/09/11
PB  - arXiv
DO  - 10.48550/arxiv.2609.13433
UR  - https://arxiv.org/abs/2609.13433
AB  - In this study, we present the full (97.3\% complete) 0.8--12.5 μm spectral energy distribution (SED) of an L/T transition object, CWISE J210640.16+250729.0 (CW2106), using the James Webb Space Telescope (JWST). We provide a full characterization of the host star's elemental abundances and age. We empirically derive the bolometric luminosity (L_bol≈−4.825 textupL_⊙) of CW2106, and obtain estimates of its mass (M≈50−62 M_Jup), radius (R≈0.83−0.87 R_Jup), effective temperature (T_eff≈1213 K), and surface gravity (log g≈5.28 dex). We find the near-infrared (near-IR) spectrum ($0.8-2.5 ~μ$m) is best reproduced with cloudy atmospheric models while the mid-infrared (mid-IR) spectrum ($5-12.5 ~μ$m) is best reproduced with cloudless models. This suggests a cloud layer restricted to only the deepest observable parts of the atmosphere and is qualified by the lack of a 9 μm silicate feature. Making use of the Mg/Si ratio of the primary, alongside thermochemical models, we predict the clouds in CW2106 to be composed primarily of enstatite (MgSiO_3), removing ∼23% of the bulk oxygen out of the atmosphere. Future retrieval studies will be able to help investigate the existence and full impact of these cloud species.
ER  -