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Table 4
S/N values to detect a secondary eclipse assuming Cycle 1 observations.
| Case | S/N Cycle 1 eclipses (MIRI F1280W) | S/N Cycle 1 eclipses (MIRI F1500W) | ||
|---|---|---|---|---|
| 1b airless 0 albedo | 8.7 | 9.0 | ||
| 1b airless 0.2 albedo | 7.6 | 7.9 | ||
| 1b 0.1 bar CO2 | 4.3 | 2.3 | ||
| 1b 1 bar CO2 | 2.7 | 2.1 | ||
| 1b 10 bar CO2 | 2.2 | 1.9 | ||
| 1b 1 bar H2O | 5.6 | 5.0 | ||
| 1b 3 bar H2O | 5.5 | 5.0 | ||
| 1b 10 bar H2O | 5.5 | 4.9 | ||
| 1c airless 0.2 albedo | 5.5 | |||
| 1c 0.1 bar CO2 | 1.3 | |||
| 1c 1 bar CO2 | 0.9 | |||
| 1c 10 bar CO2 | 1.1 | |||
| 1c 10 bar H2O | 3.2 | |||
Notes. Here we corrected the S/N to adjust the Kurucz stellar flux of TRAPPIST-1 in the F1500W MIRI filter to the observed value (Greene et al. 2023; Zieba et al. 2023).
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