Table 1
1: Fraction of eclipsing binaries in double and triple systems and transiting giant planets, among 106 simulated systems, which present either the primary or secondary or both primary and secondary eclipse(s), as seen from the Earth. 2: Global occurrence rate for these systems, as reported in the literature. 3: Occurrence rate (fraction × overall likelihood × spectral type correction) of secondary-only, primary-only, and both primary and secondary eclipse(s) for the different configurations of system. 4: Number of KOIs that might be mimicked by a secondary-only system according to the Kepler-capability detection model of Fressin et al. (2013).
| 1. | Binary system | Hierarchical triple | Nonhierarchical triple | Giant planet |
| Fraction of secondary-only | 0.126% ± 0.004% | 0.227% ± 0.005% | 0.391% ± 0.006% | 0.091% ± 0.003% |
| Fraction of primary-only | 0.129% ± 0.004% | 0.228% ± 0.005% | 0.394% ± 0.006% | 0.482% ± 0.007% |
| Fraction of primary and secondary | 0.633% ± 0.008% | 2.153% ± 0.015% | 3.632% ± 0.019% | 1.703% ± 0.013% |
| Total fraction of primary and/or secondary | 0.888% ± 0.016% | 2.608% ± 0.025% | 4.417% ± 0.031% | 2.276% ± 0.023% |
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| 2. | Binary system | Hierarchical triple | Nonhierarchical triple | Giant planet |
| Overall likelihood | 33% ± 2%† | 11% ± 2% × 76%† | 11% ± 2% × 24%† | 9.7% ± 1.3%‡ |
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| 3. | Binary system | Hierarchical triple | Nonhierarchical triple | Giant planet |
| Occurrence of secondary-only | 0.043% ± 0.004% | 0.019% ± 0.007% | 0.011% ± 0.003% | 0.009% ± 0.001% |
| Occurrence of primary-only | 0.044% ± 0.004% | 0.020% ± 0.007% | 0.011% ± 0.003% | 0.047% ± 0.007% |
| Occurrence of primary and secondary | 0.215% ± 0.016% | 0.184% ± 0.062% | 0.099% ± 0.025% | 0.165% ± 0.023% |
| Total occurrence of primary and/or secondary | 0.302% ± 0.022% | 0.223% ± 0.075% | 0.120% ± 0.031% | 0.221% ± 0.031% |
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| 4. | Binary system | Hierarchical triple | Nonhierarchical triple | Giant planet |
| Number of mimicked KOIs | 22.6 ± 4.4 | 10.0 ± 2.7 | 10.1 ± 2.7 | 0.4 ± 0.4 |
Notes.
As reported by Raghavan et al. (2010);
as reported by Mayor et al. (2011) for giant planets at any orbital period (mpsini > 100 M⊕).
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