MINDS
Astronomy and Astrophysics, vol. 703, pp. A18
Abstract
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.
Authors 24
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Affiliation as printed
Centro de Astrobiología (CAB), CSIC-INTA, ESAC Campus
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Affiliation as printed
Department of Astrophysics/IMAPP, Radboud University
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Affiliation as printed
Kapteyn Astronomical Institute, Rijksuniversiteit Groningen
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University of Liège · KU Leuven
Affiliation as printed
Institute of Astronomy, KU Leuven
STAR Institute, Université de Liège
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Affiliation as printed
Centro de Astrobiología (CAB), CSIC-INTA, ESAC Campus
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Affiliation as printed
Kapteyn Astronomical Institute, Rijksuniversiteit Groningen
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Leiden University · Max Planck Society · Max Planck Institute for Extraterrestrial Physics · Leiden Observatory
Affiliation as printed
Leiden Observatory, Leiden University
Max-Planck Institut für Extraterrestrische Physik (MPE)
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Max Planck Institute for Astronomy
Affiliation as printed
Max-Planck-Institut für Astronomie (MPIA)
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Affiliation as printed
Department of Astrophysics/IMAPP, Radboud University
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Leiden University · Leiden Observatory
Affiliation as printed
Leiden Observatory, Leiden University
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University of Vienna · ETH Zurich · Institute for Particle Physics and Astrophysics
Affiliation as printed
Dept. of Astrophysics, University of Vienna
ETH Zürich, Institute for Particle Physics and Astrophysics
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Centre National de la Recherche Scientifique · Université Paris Cité · Commissariat à l'Énergie Atomique et aux Énergies Alternatives · Université Paris-Saclay · Astrophysique, Instrumentation et Modélisation
Affiliation as printed
Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM
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Astronomical Observatory of Capodimonte · National Institute for Astrophysics
Affiliation as printed
INAF – Osservatorio Astronomico di Capodimonte
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ETH Zurich · Institute for Particle Physics and Astrophysics
Affiliation as printed
ETH Zürich, Institute for Particle Physics and Astrophysics
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Centre National de la Recherche Scientifique · Université Paris Sciences et Lettres · Observatoire de Paris · Sorbonne Université · Laboratoire d’études spatiales et d’instrumentation en astrophysique
Affiliation as printed
LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris
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Affiliation as printed
Institute of Astronomy, KU Leuven
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Affiliation as printed
Department of Physics and Astronomy, University of Exeter
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Austrian Academy of Sciences · University of Groningen · Graz University of Technology · Space Research Institute
Affiliation as printed
Kapteyn Astronomical Institute, Rijksuniversiteit Groningen
Space Research Institute, Austrian Academy of Sciences
TU Graz, Fakultät für Mathematik, Physik und Geodäsie
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University of Copenhagen · Max Planck Institute for Astronomy
Affiliation as printed
Max-Planck-Institut für Astronomie (MPIA)
Niels Bohr Institute, University of Copenhagen, NBB BA2
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Max Planck Institute for Astronomy
Affiliation as printed
Max-Planck-Institut für Astronomie (MPIA)
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Max Planck Institute for Astronomy
Affiliation as printed
Max-Planck-Institut für Astronomie (MPIA)
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Leiden University · Leiden Observatory
Affiliation as printed
Leiden Observatory, Leiden University
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Affiliation as printed
Centro de Astrobiología (CAB), CSIC-INTA, ESAC Campus
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Affiliation as printed
Department of Astronomy, Oskar Klein Centre; Stockholm University;
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