Table 3
Detection prospects for Kepler-1625 b-like and Kepler-1708 b-like exomoon candidates with the ET mission.
| System | Observing baseline | Transit epochs | mV = 10 | mV = 11 | mV = 12 | mV = 13 | mV = 14 |
|---|---|---|---|---|---|---|---|
| Kepler-1625 b-like | 4 years | 6 | TTVs | TTVs | TTVs | – | – |
| Kepler-1625 b-like | 8 years | 11 | TTVs | TTVs | TTVs | TTVs | TTVs |
| Kepler-1708 b-like | 4 years | 2 | – | – | – | – | – |
| Kepler-1708 b-like | 8 years | 4 | TTVs/TDVs/TRVs/TFVs TTVs/TDVs/TRVs/TFVs* TTVs/TDVs* TTVs/TDVs* | TTVs | |||
Names. Columns 4–8 listing the specific MCB-based methods (e.g., TTVs, TDVs) indicate that the simulated exomoon candidate was successfully detected with a significance level of > 3σ using that specific method. The symbol “–” indicates that all methods failed to detect the exomoon signal (<3σ). An asterisk (*) denotes cases where the detection method works in some cases and fails in other cases due to the random nature of the simulation. The simulation parameters are based on the configurations described in Sect. 4.6, scaled to different host star magnitudes (mV).
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