Table 2.
Sets of observational constraints to calibrate models.
| Model name | Observational constraints | Reference |
|---|---|---|
| includes: | ||
| Δνδν | ΔνAΔνB (lin. regr. on νℓ = 0, 1, 2, 3) | dM10 |
| ⟨δν02, A⟩ ⟨δν02, B⟩ | ||
| r10 | Individual r10(n) of each star | dM10 |
| r02 | Individual r02(n) of each star | dM10 |
| r13 | Individual r13(n) of each star | dM10 |
| R, Teff | RA, RB | K17 |
| Teff, A ( † ), Teff, B ( † ) | K17 | |
| Z/X|S = 0.0307 ± 0.0021 ( ‡ ) | PdM08 | |
| Mfrac, Rratio | MB/(MA + MB) | K16 |
| RA/RB | K17 | |
| LA, LB | K17 | |
| Z/X|S = 0.0307 ± 0.0021 ( ‡ ) | PdM08 | |
| M, R |
 ,  |
K16 |
| RA, RB | K17 | |
| LA, LB | K17 | |
| Z/X|S = 0.0307 ± 0.0021 ( ‡ ) | PdM08 | |
| Z/XBTK08 | Z/X|S = 0.0255 ± 0.0018 ( * ) | BTK08 |
| GN93 | Z/X|S = 0.0415 ± 0.0029 (✠) | PdM08 |
Notes. If not given here, values of the constraints can be found in Table 1.
References. dM10 (de Meulenaer et al. 2010); K16 (Kervella et al. 2016); K17 (Kervella et al. 2017b); ( † )K17 derived σTeff ∼ 20 K, we instead adopted a conservative error of 60 K; ( ‡ )assuming the AGSS09 solar distribution of elements and [Fe/H] = +0.24 ± 0.03 from PdM08 (Porto de Mello et al. 2008); ( + )K16 derived σM ∼ 0.003 M⊙; we revised the error to 0.03 M⊙ to enable the unbiased performance of our local optimisation method (see Sect. 3); ( * )assuming the AGSS09 solar distribution of elements and [Fe/H] = +0.16 ± 0.05 from BTK08 (Bigot et al. 2008); (✠)assuming the GN93 solar distribution of elements and [Fe/H] = +0.24 ± 0.03 from PdM08.
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