학술논문
MINDS. The DR Tau disk I: combining JWST-MIRI data with high-resolution CO spectra to characterise the hot gas
Document Type
Working Paper
Author
Temmink, Milou; van Dishoeck, Ewine F.; Grant, Sierra L.; Tabone, Benoit; Gasman, Danny; Christiaens, Valentin; Samland, Matthias; Argyriou, Ioannis; Perotti, Giulia; Guedel, Manuel; Henning, Thomas; Lagage, Pierre-Oliver; Abergel, Alian; Absil, Olivier; Barrado, David; Garatti, Alessio Caratti o; Glauser, Adrian M.; Kamp, Inga; Lahuis, Fred; Olofsson, Goeran; Ray, Tom P.; Scheithauer, Silvia; Vandenbussche, Bart; Waters, Rens L. B. F. M.; Arabhavi, Aditya M.; Jang, Hyerin; Kanwar, Jayatee; Morales-Calderon, Maria; Rodgers-Lee, Donna; Schreiber, Juergen; Schwarz, Kamber; Colina, Luis
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Abstract
The MRS mode of the JWST-MIRI instrument has been shown to be a powerful tool to characterise the molecular gas emission of the inner region of planet-forming disks. Here, we analyse the spectrum of the compact T-Tauri disk DR Tau, which is complemented by high spectral resolution (R~60000-90000) CO ro-vibrational observations. Various molecular species, including CO, CO$_2$, HCN, and C$_2$H$_2$ are detected in the JWST-MIRI spectrum, for which excitation temperatures of T~325-900 K are retrieved using LTE slab models. The high-resolution CO observations allow for a full treatment of the line profiles, which show evidence for two components of the main isotopologue, $^{12}$CO: a broad component tracing the Keplerian disk and a narrow component tracing a slow disk wind. Rotational diagrams yield excitation temperatures of T>725 K for CO, with consistently lower temperatures found for the narrow components, suggesting that the disk wind is launched from a larger distance. The inferred excitation temperatures for all molecules suggest that CO originates from the highest atmospheric layers close to the host star, followed by HCN and C$_2$H$_2$, which emit, together with $^{13}$CO, from slightly deeper layers, whereas the CO$_2$ originates from even deeper inside or further out in the disk. Additional analysis of the $^{12}$CO line wings hint at a misalignment between the inner (i~20 degrees) and outer disk (i~5 degrees). Finally, we emphasise the need for complementary high-resolution CO observations, as in combination with the JWST-MIRI observations they can be used to characterise the CO kinematics and the physical and chemical conditions of the other observed molecules with respect to CO.
Comment: Accepted for publication in Astronomy & Astrophysics on 20/03/2024
Comment: Accepted for publication in Astronomy & Astrophysics on 20/03/2024