MINDS
Authors: Gasman Danny , van Dishoeck Ewine F. , Grant Sierra L. , Temmink Milou , Tabone Benoît , Henning Thomas , Kamp Inga , Güdel Manuel , Lagage Pierre-Olivier , Perotti Giulia , Christiaens Valentin , Samland Matthias , Arabhavi Aditya M. , Argyriou Ioannis , Abergel Alain , Absil Olivier , Barrado David , Boccaletti Anthony , Bouwman Jeroen , Caratti o Garatti Alessio , Geers Vincent , Glauser Adrian M. , Guadarrama Rodrigo , Jang Hyerin , Kanwar Jayatee , Lahuis Fred , Morales-Calderón Maria , Mueller Michael , Nehmé Cyrine , Olofsson Göran , Pantin Éric , Pawellek Nicole , Ray Tom P. , Rodgers-Lee Donna , Scheithauer Silvia , Schreiber Jürgen , Schwarz Kamber , Vandenbussche Bart , Vlasblom Marissa , Waters Rens L. B. F. M. , Wright Gillian , Colina Luis , Greve Thomas R. , Östlin Göran 
Published: September 2023

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 H2O 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 H2O lines of different excitation conditions, and the slab model fits were performed individually per region.

Results. We confidently detect CO, H2O, OH, CO2, and HCN in the emitting layers. Despite the plethora of H2O lines, the isotopo-logue H218O is not detected. Additionally, no other organics, including C2H2, are detected. This indicates that the C/O ratio could be substantially below unity, in contrast with the outer disk. The H2O emission traces a large radial disk surface region, as evidenced by the gradually changing excitation temperatures and emitting radii. Additionally, the OH and CO2 emission is relatively weak. It is likely that H2O is not significantly photodissociated, either due to self-shielding against the stellar irradiation, or UV shielding from small dust particles. While H2O 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 H2O 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.