Table 2
Simulation parameters.
| Fig. 2 | Fig. 4 | Fig. 5 | Fig. 6 | |
|---|---|---|---|---|
| F⋆ | 10Jy | 10Jy | 10Jy | |
| δt | 100 s | 100 s | 100 s | |
| Δt | 3h | 3h | 3h | |
| Tr | 0–10% | 5% | 5% | |
| Tlab | 300K | 300K | 300K | |
| D | 8 | 8 | 8 | 8 |
| Ntel | 2 | 2 | 2 | 2 |
| Δλ/λ | 0.23 | 0.23 | 0.23 | 0.23 |
| λ/δλ | 100 | 100 | 100 | 100 |
| λB | J/H/K/L | I/K | K | I/J/H/K/L |
| Strehl | 98 | 98 | 88/98 | |
| | B| | 100/200 m | 100/200 m | ||
| npoly | 3–7–11 | 11 |
Notes. F⋆ is flux of the stellar host. δt is the integration time of individual frames while Δt the total integration time. Tr is the total transmission of the instrument, D is the diameter of the telescopes and Ntel is the number of telescopes. Δλ/λ the spectral bandwidth and λ/δλ is the spectral resolution. λB is the name of the spectral band. |B| is the projected baseline length, while npoly is the polynomial order used for stellar light post processing.
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