Table 7
Number of M and K dwarf exoplanetary transit light curves observed by TESS forecasted to contain observable starspot anomalies.
| Spectral | Starspot filling | Forecasted TESS light |
|---|---|---|
| type | factor (%) | curves containing starspots |
| Uniform distribution | ||
| M dwarf | 40% ± 10% | 249 ± 32 |
| M dwarf | 20% ± 5% | 172 ± 25 |
| M dwarf | 4.0% ± 1.0% | 63 ± 11 |
| M dwarf | 2.0% ± 0.5% | 49 ± 10 |
| M dwarf | 0.4% ± 0.1% | 11 ± 5 |
| M dwarf | 0.20% ± 0.05% | 9 ± 5 |
| 64 ± 9 | ||
| K dwarf | 30% ± 10% | 103 ± 18 |
| K dwarf | 15% ± 5% | 67 ± 13 |
| K dwarf | 3.0% ± 1.0% | 25 ± 6 |
| K dwarf | 1.5% ± 0.5% | 20 ± 5 |
| K dwarf | 0.3% ± 0.1% | 6 ± 3 |
| K dwarf | 0.15% ± 0.05% | 5 ± 3 |
| 23 ± 4 | ||
| Polar distribution | ||
| M dwarf | 40% ± 10% | 88 ± 15 |
| M dwarf | 20% ± 5% | 80 ± 14 |
| M dwarf | 4.0% ± 1.0% | 58 ± 9 |
| M dwarf | 2.0% ± 0.5% | 40 ± 8 |
| M dwarf | 0.4% ± 0.1% | 11 ± 5 |
| M dwarf | 0.20% ± 0.05% | 11 ± 5 |
| 37 ± 6 | ||
| K dwarf | 30% ± 10% | 47 ± 8 |
| K dwarf | 15% ± 5% | 33 ± 7 |
| K dwarf | 3.0% ± 1.0% | 19 ± 5 |
| K dwarf | 1.5% ± 0.5% | 14 ± 4 |
| K dwarf | 0.3% ± 0.1% | 4 ± 2 |
| K dwarf | 0.15% ± 0.05% | 4 ± 2 |
| 12 ± 2 | ||
| Mid-latitude distribution | ||
| M dwarf | 40% ± 10% | 138 ± 20 |
| M dwarf | 20% ± 5% | 116 ± 18 |
| M dwarf | 4.0% ± 1.0% | 61 ± 11 |
| M dwarf | 2.0% ± 0.5% | 49 ± 9 |
| M dwarf | 0.4% ± 0.1% | 10 ± 5 |
| M dwarf | 0.20% ± 0.05% | 7 ± 5 |
| 47 ± 7 | ||
| K dwarf | 30% ± 10% | 64 ± 12 |
| K dwarf | 15% ± 5% | 50 ± 10 |
| K dwarf | 3.0% ± 1.0% | 25 ± 6 |
| K dwarf | 1.5% ± 0.5% | 26 ± 5 |
| K dwarf | 0.3% ± 0.1% | 5 ± 3 |
| K dwarf | 0.15% ± 0.05% | 3 ± 2 |
| 21 ± 4 | ||
Notes. These combine the results presented in Tables 4, 5, and 6 with the results from Barclay et al. (2018). The weighted mean of the forecasted number of transits of the different starspot filling factors is given in bold.
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