Table 6
Probability of detecting at least one magma ocean planet with atmospheric emissivity ϵ = 0.01, based on fluxdensity calculations performed with brightness temperatures from Lupu et al. (2014; see Fig. 7).
| P (%) – 5 h | P (%) – 50 h | ||
|---|---|---|---|
| Filter | SA | ϵ = 0.01 | ϵ = 0.01 |
| L56 | β Pictoris | 4.4 | 35.7 |
| Tucana-Horologium | – | 14.0 | |
| Columba | – | 16.5 | |
| TW Hydrae | – | 7.1 | |
| L10 | β Pictoris | 26.4 | 86.1 |
| Tucana-Horologium | – | 25.3 | |
| Columba | – | 28.6 | |
| TW Hydrae | – | 13.1 | |
| E22 | β Pictoris | 0.1 | 7.1 |
| Tucana-Horologium | – | 0.4 | |
| Columba | – | 0.4 | |
| TW Hydrae | – | 0.04 | |
| E38 | β Pictoris | – | 5.1 |
| Tucana-Horologium | – | 0.06 | |
Notes. Detection likelihoods are shown for the most promising stellar targets, for different integration times (5 and 50 h per star) and instruments (L56: LIFE 5.6 μm, L10: LIFE 10 μm, E22: ELT 2.2 μm, E38: ELT 3.8 μm). We do not show detection probabilitiesfor ELT 11.6 μm, as it is not able to detect any magma ocean planets (cf. Fig. 7).
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