MINDS. Abundant water and varying C/O across the disk of Sz 98 as seen by JWST/MIRI

Autor(en)
Danny Gasman, Ewine F. van Dishoeck, Sierra L. Grant, Milou Temmink, Benoit Tabone, Thomas Henning, Inga Kamp, Manuel Güdel, Pierre-Olivier Lagage, Giulia Perotti, Valentin Christiaens, Matthias Samland, Aditya M. Arabhavi, Ioannis Argyriou, Alain Abergel, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alessio Caratti o Garatti, Vincent Geers, Adrian M. Glauser, Rodrigo Guadarrama, Hyerin Jang, Jayatee Kanwar, Fred Lahuis, Maria Morales-Calderón, Michael Mueller, Cyrine Nehmé, Göran Olofsson, Éric Pantin, Nicole Pawellek, Tom P. Ray, Donna Rodgers-Lee, Silvia Scheithauer, Jürgen Schreiber, Kamber Schwarz, Bart Vandenbussche, Marissa Vlasblom, Rens L.~B.~F.~M. Waters, Gillian Wright, Luis Colina, Thomas R. Greve, Göran Östlin
Abstrakt

Context. The Mid-InfraRed Instrument (MIRI) Medium Resolution Spectrometer (MRS) on board the James Webb Space Telescope (JWST) allows us to probe the inner regions of protoplanetary disks, where the elevated temperatures result in an active chemistry and where the gas composition may dictate the composition of planets forming in this region. The disk around the classical T Tauri star Sz 98, which has an unusually large dust disk in the millimetre with a compact core, was observed with the MRS, and we examine its spectrum here. Aims. We aim to explain the observations and put the disk of Sz 98 in context with other disks, with a focus on the H

2O emission through both its ro-vibrational and pure rotational emission. Furthermore, we compare our chemical findings with those obtained for the outer disk from Atacama Large Millimeter/submillimeter Array (ALMA) observations. Methods. In order to model the molecular features in the spectrum, the continuum was subtracted and local thermodynamic equilibrium (LTE) slab models were fitted. The spectrum was divided into different wavelength regions corresponding to H

2O lines of different excitation conditions, and the slab model fits were performed individually per region. Results. We confidently detect CO, H

2O, OH, CO

2, and HCN in the emitting layers. Despite the plethora of H

2O lines, the isotopologue H

2 18O is not detected. Additionally, no other organics, including C

2H

2, are detected. This indicates that the C/O ratio could be substantially below unity, in contrast with the outer disk. The H

2O emission traces a large radial disk surface region, as evidenced by the gradually changing excitation temperatures and emitting radii. Additionally, the OH and CO

2 emission is relatively weak. It is likely that H

2O is not significantly photodissociated, either due to self-shielding against the stellar irradiation, or UV shielding from small dust particles. While H

2O is prominent and OH is relatively weak, the line fluxes in the inner disk of Sz 98 are not outliers compared to other disks. Conclusions. The relative emitting strength of the different identified molecular features points towards UV shielding of H

2O in the inner disk of Sz 98, with a thin layer of OH on top. The majority of the organic molecules are either hidden below the dust continuum, or not present. In general, the inferred composition points to a sub-solar C/O ratio (<0.5) in the inner disk, in contrast with the larger than unity C/O ratio in the gas in the outer disk found with ALMA.

Organisation(en)
Institut für Astrophysik
Externe Organisation(en)
Katholieke Universiteit Leuven, Leiden University, Max-Planck-Institut für extraterrestrische Physik, Université Paris Saclay, Max-Planck-Institut für Astronomie, University of Groningen, Eidgenössische Technische Hochschule Zürich, Université de Liège, Centro de Astrobiología (CAB), Université Paris VII - Paris-Diderot, INAF-Osservatorio Astronomico di Capodimonte, Dublin Institute for Advanced Studies, The Royal Observatory, Edinburgh, Radboud University, Österreichische Akademie der Wissenschaften (ÖAW), Technische Universität Graz, SRON Netherlands Institute for Space Research , Stockholm University, Hungarian Academy of Sciences, MTA Társadalomtudományi Kutatóközpont, Centro de Astrobiología (CSIC-INTA), Technical University of Denmark (DTU)
Journal
Astronomy & Astrophysics
Band
679
Anzahl der Seiten
17
ISSN
0004-6361
DOI
https://doi.org/10.1051/0004-6361/202347005
Publikationsdatum
11-2023
Peer-reviewed
Ja
ÖFOS 2012
103004 Astrophysik
Schlagwörter
ASJC Scopus Sachgebiete
Astronomy and Astrophysics, Space and Planetary Science
Link zum Portal
https://ucrisportal.univie.ac.at/de/publications/2849538d-3e15-4c64-a07b-6c6cbbf8072b