Table 2
Non-linear limb-darkening coefficients obtained by linear interpolation on the tables provided by Claret & Bloemen (2011) based on PHOENIX atmosphere models.
| Filter | a1 | a2 | a3 | a4 | L3 |
|
|
|||||
| Kepler | 0.473a | 0.192a | − | − | 0.0276 |
| Kepler | 0.801 | −0.676 | 1.053 | −0.388 | 0.0276 |
| Strömgren u | 0.910 | −1.006 | 1.388 | −0.355 | 0.0045 |
| Strömgren v | 0.863 | −0.767 | 1.872 | −0.617 | 0.0102 |
| Strömgren b | 0.698 | −1.206 | 1.572 | −0.599 | 0.0180 |
| Strömgren y | 0.758 | −0.663 | 1.203 | −0.454 | 0.0227 |
| Johnson U | 1.085 | −1.412 | 1.721 | −0.466 | 0.0053 |
| Johnson B | 0.754 | −0.937 | 1.734 | −0.641 | 0.0137 |
| Johnson V | 0.742 | −0.602 | 1.134 | −0.434 | 0.0216 |
| Cousins R | 0.796 | −0.632 | 0.993 | −0.378 | 0.0294 |
| Cousins I | 0.853 | −0.746 | 0.963 | −0.363 | 0.0360 |
| SDSS i′ | 0.829 | −0.688 | 0.935 | −0.354 | 0.0343b |
| SDSS z′ | 0.861 | −0.807 | 0.967 | −0.360 | 0.0425b |
Notes. The last column gives the fraction of flux due to the visual companion detected by Daemgen et al. (2009).
Values are based on magnitude differences directly measured by Daemgen et al. (2009).
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