Table 1
Observational constraints of the targets from our testing set.
| Nickname | KIC | Teff (K) | [Fe/H] (dex) | L (L⊙) | νmax (µHz) | References |
|---|---|---|---|---|---|---|
| (K) | (dex) | (L⊙) | (µHz) | |||
| Model A | 5775.1 ± 90 | 0.027 ± 0.10 | 1.003 ± 0.191 | 1 | ||
| Model B | 6725.8 ± 100 | 0.027 ± 0.10 | 3.862 ± 0.425 | 1 | ||
| Model C | 6485.8 ± 100 | 0.027 ± 0.10 | 6.399 ± 0.704 | 1 | ||
| Model D | 6431.9 ± 100 | 0.027 ± 0.10 | 2.969 ± 0.564 | 1 | ||
| Model E | 6227.0 ± 100 | 0.027 ± 0.10 | 5.075 ± 0.558 | 1 | ||
| Model F | 6103.3 ± 100 | 0.027 ± 0.10 | 2.137 ± 0.406 | 1 | ||
| Model G | 5861.0 ± 90 | 0.027 ± 0.10 | 0.990 ± 0.188 | 1 | ||
| Sun | 5772 ± 85 | 0.00 ± 0.10 | 1.00 ± 0.03 | 2 | ||
| α Cen A | 5795 ± 19 | 0.24 ± 0.01 | 1.521 ± 0.015 | 3 | ||
| α Cen B | 5231 ± 21 | 0.24 ± 0.01 | 0.503 ± 0.007 | 3 | ||
| Kepler-93 | 3544595 | 5718 ± 100 | −0.18 ± 0.10 | 0.82 ± 0.03 | 4 | |
| Nunny | 6116048 | 6033 ± 100 | −0.23 ± 0.10 | 1.85 ± 0.07 | 2126.9 ± 5.3 | 4 |
| Saxo2 | 6225718 | 6203 ± 100 | −0.17 ± 0.10 | 2.13 ± 0.08 | 2364.2 ± 4.8 | 5 |
| Baloo | 6508366 | 6331 ± 100 | −0.05 ± 0.10 | 6.78 ± 0.27 | 958.3 ± 4.1 | 5 |
| Doris | 8006161 | 5488 ± 100 | 0.34 ± 0.10 | 0.69 ± 0.03 | 3574.7 ± 11.0 | 4 |
| Arthur | 8379927 | 6067 ± 150 | −0.10 ± 0.15 | – | 2795.3 ± 6.0 | 6 |
| Carlsberg | 9139151 | 6043 ± 100 | 0.05 ± 0.10 | 1.60 ± 0.06 | 2690.4 ± 11.8 | 5 |
| Punto | 9139163 | 6400 ± 60 | 0.15 ± 0.10 | 3.68 ± 0.13 | 1729.8 ± 6.1 | 5 |
| Pinocha | 10454113 | 6177 ± 100 | −0.07 ± 0.10 | – | 2357.2 ± 8.7 | 4 |
| Tinky | 11253226 | 6642 ± 100 | −0.08 ± 0.10 | 4.44 ± 0.16 | 1590.6 ± 8.7 | 4 |
| Dushera | 12009504 | 6179 ± 100 | −0.08 ± 0.10 | 2.70 ± 0.11 | 1865.6 ± 7.0 | 4 |
| 16 Cyg A | 12069424 | 5839 ± 42 | 0.096 ± 0.026 | 1.56 ± 0.02 | 7 | |
| 16 Cyg B | 12069449 | 5809 ± 39 | 0.052 ± 0.021 | 1.27 ± 0.02 | 7 | |
| Barney | 12258514 | 5964 ± 60 | 0.00 ± 0.10 | 2.95 ± 0.11 | 1512.7 ± 3.1 | 4 |
Notes. (1) Sonoi et al. (2015); (2) frequencies from measurement n°01 of Salabert et al. (2015) and Teff from Prša et al. (2016), the uncertainty of the classical constraints is adapted to match the expectation from a Kepler observation; (3) see Salmon et al. (2021) and references therein; (4) Lund et al. (2017); (5) frequencies and νmax from Lund et al. (2017), Teff and [Fe/H] from Furlan et al. (2018)); (6) frequencies from Roxburgh (2017), Teff, [Fe/H], and νmax from Lund et al. (2017); (7) Teff from White et al. (2013), [Fe/H] from Ramirez et al. (2009), and L from Metcalfe et al. (2012). Models A to G are synthetic models whose classical constraints are known exactly. The uncertainty was chosen to match the expectation from a Kepler observation. The other targets are actual observations for which the luminosity was estimated using the spectroscopic parameters and Eq. (13) in JB23. The RUWE indicator of Gala flags the parallax measurement of Arthur as unreliable, and the Ks-magnitude measurement of Pinocha is unreliable as well.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.