Table 1.
Instrumental noise (with mref = 8).
| Project |  |
 |
 |
a |
|---|---|---|---|---|
| (ppm h1/2) | (ppm h1/2) | (ppm h1/2) | ||
| CoRoTa | 3.2 | 15.5 | ||
| Keplerb | 2.8 | 8.0 | 0.4 | 0.7 |
| PLATOc | 9 | 9 | 2 | 0.66 |
| TESSd | 0–60 | 60 | 10 | 0.68 |
Notes.
Appourchaux et al. (2008) and Auvergne et al. (2009); as only bright stars were considered, we did not model the additional component.
Jenkins et al. (2010a); the systematic noise is derived from the observation of the bright twin systems 16 Cyg A and B by Metcalfe et al. (2012).
Rauer et al. (2014), updated to the new configuration of PLATO with 24 telescopes and following the requirements of the mission expressed in the PLATO Definition Study Report.
Campante et al. (2016); 
= 60 ppm h1/2 is presented as the worst case; we use 
= 30 ppm h1/2 in our simulations.
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