Table 5
Stellar parameters of the PHOENIX atmospheric models used in this analysis from Allard et al. (2012b) assuming the set of solar abundances from Asplund et al. (2009).
| [m/H] = 0 | [m/H] = + 0.5 | ||
| Parameter | Nominal1 | Best fit | Best fit |
|
|
|||
|
5700 | 5300 | 5600 |
|
4900 | 4700 | 4900 |
| log ghot | 3.0 | 2.0 | 2.5 |
| log gcool | 2.5 | 2.0 | 2.5 |
|
4.37 | 2.89 | 2.31 |
|
|
|||
| Rcool/Rhot | 0.703 | 0.723 | 0.726 |
Notes. The first two models are at solar metallicity, while the third assumes super-solar metallicity. All three models are shown in Fig. 6. The parameters adopted to mimic those from Torres et al. (2009) are slightly different from those given in their paper because of the discrete sampling of the PHOENIX model grid. The last line of the table gives the ratio of stellar radii derived from the scaling factor used to normalize the spectra as a first step of the modeling.
Reference. 1Torres et al. (2009).
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