MINDS Article Swipe
M. Morales‐Calderón
,
Hyerin Jang
,
M. Aditya Arabhavi
,
Valentin Christiaens
,
D. Barrado
,
I. Kamp
,
F. Ewine van Dishoeck
,
Thomas Henning
,
L. B. F. M. Waters
,
Milou Temmink
,
M. Güdel
,
Pierre-Olivier Lagage
,
A. Caratti o Garatti
,
M. Adrian Glauser
,
P. C. Ray
,
Riccardo Franceschi
,
Danny Gasman
,
Linda Grant
,
Till Kaeufer
,
J. S. Kanwar
,
Giulia Perotti
,
M. Samland
,
Kamber R. Schwarz
,
Marissa Vlasblom
,
L. Colina
,
Göran Östlin
·
YOU?
·
· 2025
· Open Access
·
· DOI: https://doi.org/10.1051/0004-6361/202555621
YOU?
·
· 2025
· Open Access
·
· DOI: https://doi.org/10.1051/0004-6361/202555621
Context. The chemistry of disks around brown dwarfs (BDs) remains largely unexplored due to their faintness. Despite the efforts performed with Spitzer, we have far less understanding of planet formation, chemical composition, disk structure, and evolution in disks around BDs compared to their more massive counterparts (T Tauri and Herbig Ae/Be stars), which are more readily studied due to their greater brightness. Recent JWST observations, with up to an order of magnitude improvement in both spectral and spatial resolution, have shown that these systems are chemically rich, offering valuable insights into giant planet formation. Aims. As part of the MIRI mid-INfrared Disk Survey (MINDS) JWST guaranteed time program, we aim to characterize the gas and dust composition of the disk around the brown dwarf [NC98] Cha HA 1, hereafter Cha H α 1, in the mid-infrared. Methods. We obtained data from the MIRI Medium Resolution Spectrometer (MRS) from 4.9 to 28 μm ( R ∼ 1500–3500; FWHM ∼ 0.2″–1.2″). We used the dust fitting tool DuCK to investigate the dust composition and grain sizes, while we identified and fit molecular emission in the spectrum using slab models. Results. Compared with disks around very low mass stars, clear silicate emission features are seen in this BD disk. In addition, JWST reveals a plethora of hydrocarbons, including C 2 H 2 , 13 CCH 2 , CH 3 , CH 4 , C 2 H 4 , C 4 H 2 , C 3 H 4 , C 2 H 6 , and C 6 H 6 which suggest a disk with a gas C/O > 1. Additionally, we detected CO 2 , 13 CO 2 , HCN, H 2 , and H 2 O. Notably, CO and OH are absent from the spectrum. The dust is dominated by large ∼4 μm size amorphous silicates (MgSiO 3 ). We inferred a small dust mass fraction (> 10%) of 5 μm size crystalline forsterite. We did not detect any polycyclic aromatic hydrocarbons. Conclusions. The mid-infrared spectrum of Cha H α 1 shows the most diverse chemistry seen to date in a BD protoplanetary disk, consisting of a strong dust feature, 12 carbon-bearing molecules plus H 2 , and water. The diverse molecular environment offers a unique opportunity to test our understanding of BD disk chemistry and how it affects the possible planets forming in them.
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Metadata
- Type
- article
- Language
- en
- Landing Page
- https://doi.org/10.1051/0004-6361/202555621
- OA Status
- hybrid
- References
- 88
- Related Works
- 10
- OpenAlex ID
- https://openalex.org/W4414053458
All OpenAlex metadata
Raw OpenAlex JSON
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https://openalex.org/W4414053458Canonical identifier for this work in OpenAlex
- DOI
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https://doi.org/10.1051/0004-6361/202555621Digital Object Identifier
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MINDSWork title
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articleOpenAlex work type
- Language
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enPrimary language
- Publication year
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2025Year of publication
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2025-09-08Full publication date if available
- Authors
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M. Morales‐Calderón, Hyerin Jang, M. Aditya Arabhavi, Valentin Christiaens, D. Barrado, I. Kamp, F. Ewine van Dishoeck, Thomas Henning, L. B. F. M. Waters, Milou Temmink, M. Güdel, Pierre-Olivier Lagage, A. Caratti o Garatti, M. Adrian Glauser, P. C. Ray, Riccardo Franceschi, Danny Gasman, Linda Grant, Till Kaeufer, J. S. Kanwar, Giulia Perotti, M. Samland, Kamber R. Schwarz, Marissa Vlasblom, L. Colina, Göran ÖstlinList of authors in order
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https://doi.org/10.1051/0004-6361/202555621Publisher landing page
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YesWhether a free full text is available
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hybridOpen access status per OpenAlex
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https://doi.org/10.1051/0004-6361/202555621Direct OA link when available
- Cited by
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0Total citation count in OpenAlex
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88Number of works referenced by this work
- Related works (count)
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10Other works algorithmically related by OpenAlex
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| abstract_inverted_index.( | 152 |
| abstract_inverted_index., | 219, 223, 226, 229, 234, 239, 244, 249, 270, 274, 278, 363 |
| abstract_inverted_index.1 | 337 |
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| abstract_inverted_index.3 | 225, 241, 304 |
| abstract_inverted_index.4 | 228, 233, 236, 243 |
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| abstract_inverted_index.6 | 248, 252, 254 |
| abstract_inverted_index.C | 215, 230, 235, 240, 245, 251 |
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| abstract_inverted_index.(T | 46 |
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| abstract_inverted_index.1, | 127, 132 |
| abstract_inverted_index.1. | 264 |
| abstract_inverted_index.12 | 357 |
| abstract_inverted_index.13 | 220, 271 |
| abstract_inverted_index.28 | 150 |
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| abstract_inverted_index.BD | 204, 348, 379 |
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| abstract_inverted_index.it | 384 |
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| abstract_inverted_index.α | 131, 336 |
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| abstract_inverted_index.The | 1, 292, 330, 366 |
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| abstract_inverted_index.did | 322 |
| abstract_inverted_index.due | 12, 57 |
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| abstract_inverted_index.our | 376 |
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| abstract_inverted_index.∼ | 154, 157 |
| abstract_inverted_index.> | 263 |
| abstract_inverted_index.10%) | 314 |
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| abstract_inverted_index.DuCK | 165 |
| abstract_inverted_index.FWHM | 156 |
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| abstract_inverted_index.JWST | 63, 104, 208 |
| abstract_inverted_index.MIRI | 99, 142 |
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| abstract_inverted_index.data | 139 |
| abstract_inverted_index.date | 345 |
| abstract_inverted_index.disk | 32, 119, 258, 380 |
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| abstract_inverted_index.have | 23, 79 |
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| abstract_inverted_index.Compared | 188 |
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| abstract_inverted_index.Notably, | 283 |
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