Table 1
Astrophysical and instrumental parameters for our baseline scenario.
| Parameter | Value | Description |
|
|
||
| cosi | [−1, 1) | Cosine of inclination |
| Ω | [ 0, 2π) | Longitude of ascending node |
| ω | [0, 2π) | Argument of periapsis |
| ϑ | [0, 2π) | True anomaly |
| e | 0 | Eccentricitya |
| AB | [ 0, 0.8) | Bond albedob |
| Ag | [ 0, 0.1) | Geometric albedob |
|
|
||
| IWA | 5.0 mas | IWA @ λeff = 10 μmcd |
| OWA | 1′′ | OWA @ λeff = 10 μmce |
| Flim, F560W | 0.16 μJy | Sensitivity limit (λeff = 5.6 μm)f |
| Flim, F1000W | 0.54 μJy | Sensitivity limit (λeff = 10.0 μm)f |
| Flim, F1500W | 1.39 μJy | Sensitivity limit (λeff = 15.0 μm)f |
Notes. Values are distributed uniformly in the given ranges.
See discussion in Sect. 4.2.
See discussion in Sect. 4.1.
From Leger & Herbst (2007).
10σ detection limit in 35 000 s; modified from Glasse et al. (2015) who assumed 10 000 s to achieve these limits with JWST/MIRI.
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