Table 2
Optimized power-2 limb-darkening law parameters, c and α, and the corresponding transformed parameters, h1 and h2.
| X | Teff | log g | [Fe/H] | c | α | h1 | h2 |
|---|---|---|---|---|---|---|---|
| [K] | [cgs] | ||||||
| CH | 4000 | 1.5 | − 1.0 | 0.727 | 0.916 | 0.658 | 0.39 |
| CH | 4250 | 1.5 | − 1.0 | 0.722 | 0.841 | 0.681 | 0.40 |
| CH | 4500 | 1.5 | − 1.0 | 0.724 | 0.758 | 0.704 | 0.43 |
| CH | 4000 | 2.0 | − 2.0 | 0.759 | 0.833 | 0.667 | 0.43 |
| CH | 4250 | 2.0 | − 2.0 | 0.764 | 0.739 | 0.694 | 0.46 |
| CH | 4500 | 2.0 | − 2.0 | 0.786 | 0.634 | 0.720 | 0.51 |
| CH | 4000 | 2.0 | − 1.0 | 0.714 | 0.953 | 0.655 | 0.37 |
| CH | 4250 | 2.0 | − 1.0 | 0.717 | 0.880 | 0.673 | 0.39 |
| CH | 4500 | 2.0 | − 1.0 | 0.726 | 0.804 | 0.690 | 0.42 |
| CH | 4000 | 2.0 | − 0.5 | 0.693 | 0.911 | 0.676 | 0.37 |
Notes.The bandpass, X, is noted in thefirst column as either the filter name for the Johnson photometric system, “u_”, “g_”, etc. for the SDSS photometric system, or the two initial letters for Kepler, CHEOPS, etc. For stars that do not show strong magnetic activity, it can be assumed that h1 is accurate to ± σ1 = ±0.011 and h2 is accurate to ± σ2 = ±0.045. This is an excerpt from the complete table that is available at the CDS, provided here as a guide to its format and content.
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