Table 5
Discs around stars >0.3 M⊙ observed with MIRI-MRS to which we compare our models.
| Disc | M*/M⊙ | Age (a) / Myr |  |
 |
Reference |
|---|---|---|---|---|---|
| GW Lup | 0.46 | 2 ± 1 | 3.2 × 1018 | 2.2 × 1018 | Grant et al. (2023) |
| 6.8 × 1018(c) | |||||
| Sz 98 | 0.74 | 2±1 | 3.7 × 1018−7.5 × 1019 | 2.4 × 1018 | Gasman et al. (2023) |
| SY Cha | 0.70 | 1.5 ± 0.5 | 7.0 × 1018−3.1 × 1021 | 4.9 × 1017 | Schwarz et al. (2024) |
| AS 209 | 0.96 | 1 ± 0.5 | 4.7 × 1017−2.9 × 1019 | <5.5 × 1016 | Romero-Mirza et al. (2024b) |
| CX Tau | 0.37 | 2±1 | 4 × 1019 | 7 × 1017 | Vlasblom et al. (2025) |
| 1 × 1019 (c) | |||||
| DR Tau | 0.93 | 2±1 | 4.0 × 1017−1.6 × 1019(d) | 2.5 × 1017 | Temmink et al. (2024b,a) |
| DoAr 33 | 1.1 | 4 ± 2 | 3.2 × 1018 | 6.3 × 1017 | Colmenares et al. (2024) |
Notes. (a)Ages are mostly indicative of those typically assumed for the star forming regions where the discs are located. (b)Where a range of column densities is indicated, it corresponds to the values obtained by fitting to different sections of the spectrum or multiple components. For the other discs, one can expect up to an order of magnitude uncertainty in either direction depending on fit windows chosen and the strength of the emission. (c) Alternative estimate from. 13CO2 assuming an isotope ratio of 68. (d)Multiple-component fit, Approach III.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.