Table 1
Umbrae and penumbrae longitudes and flux residuals.
| Latitude (°) | Longitude (°) | Transit time (h) | Substructure | Flux residual (ppm) |
|---|---|---|---|---|
| −15 | 1.5 | 0.04 | Umbra | 52.0 |
| 4.5 | 0.12 | Penumbra | 27.9 | |
| 7.5 | 0.20 | Penumbra | 17.1 | |
| 9.0 | 0.24 | Umbra | 23.1 | |
| −17 | 0.4 | 0.01 | Penumbra dominant | 19.1 |
| 3.5 | 0.09 | Penumbra | 28.0 | |
| 6.8 | 0.18 | Penumbra | 32.0 | |
| 8.3 | 0.22 | Umbra | 45.4 | |
| −21 | 2.7 | −0.07 | Penumbra | 27.1 |
| 0.5 | 0.01 | Umbra | 91.6 | |
| 3.3 | 0.08 | Penumbra | 22.0 | |
| 8.5 | 0.22 | Penumbra dominant | 27.2 | |
| 10.5 | 0.27 | Penumbra dominant | 27.1 |
Notes. Flux residuals are the difference between a spotless light curve model for a 1 R⊕ planet transiting an unspotted Sun and the simulated transits at solar latitudes −15°, −17°, and −21° for the spotted Sun on October 23, 2014. Correspondence with the location of features in the grayscale image of the Sun on October 23, 2014, identifies the bumps as umbrae and penumbrae, or a combination of the two. The occultation times of umbrae and penumbrae are converted to longitude.
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