Table B.3.
Median 1σ uncertainty on the extracted parameters.
| χ2 | χ2 | χ2 |  |
 |
|
|---|---|---|---|---|---|
| 3σ | 1σ | ≤1 | ≤28.87 | ||
| % | % | % | % | % | |
| Rayleigh limit corresponding to 27 day light curve | |||||
| M⋆ (M⊙) | 0.19 | 0.11 | 0.08 | 0.07 | 0.13 |
| Teff (K) | 700 | 300 | 110 | 28 | 150 |
| log g | 0.014 | 0.008 | 0.006 | 0.005 | 0.015 |
| R (R⊙) | 0.06 | 0.04 | 0.03 | 0.0325 | 0.05 |
| L (L⊙) | 8 | 3.4 | 1.4 | 0.6 | 2.0 |
| age (Myr) | 1.7 | 1.3 | 0.85 | 0.75 | 1.7 |
| Z | 0.005 | 0.004 | 0.004 | 0.004 | 0.004 |
| Rayleigh limit corresponding to 108 day light curve | |||||
| M⋆ (M⊙) | 0.13 | 0.08 | 0.06 | 0.05 | 0.11 |
| Teff (K) | 600 | 300 | 110 | 25 | 150 |
| log g | 0.010 | 0.006 | 0.005 | 0.004 | 0.009 |
| R (R⊙) | 0.04 | 0.03 | 0.02 | 0.017 | 0.04 |
| L (L⊙) | 6.5 | 3.1 | 1.2 | 0.4 | 1.8 |
| age (Myr) | 1.2 | 0.9 | 0.7 | 0.5 | 1.6 |
| Z | 0.004 | 0.003 | 0.003 | 0.003 | 0.005 |
Notes. We note that for approaches 3 and 4 it is possible that not a single model fulfils both the stringent spectroscopic and the asteroseismic demands. The values given here are the medians of the models for which at least two theoretical pulsation spectra from different evolutionary calculations fit both constraints.
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