Table 2
Seismic gravities.
| Name | Source of data | log g seismology [cgs] |
|
|
||
| HD 45398 | CoRoT SRa04 | Not available |
| HD 49429 | CoRoT SRa01 | Not available |
| HD 49566 | CoRoT SRa01 | 2.89 ± 0.04 |
| HD 50890 | CoRoT IRa01 | 2.07 ± 0.08 |
| HD 169370 | CoRoT LRc03 | 2.32 ± 0.04 |
| HD 169751 | CoRoT LRc03 | 2.67 ± 0.07 |
| HD 170008 | CoRoT LRc03 | 3.45 ± 0.04 |
| HD 170031 | CoRoT LRc07, LRc08 | 2.47 ± 0.09 |
| HD 171427 | CoRoT LRc02 | Not available |
| HD 175679 | CoRoT SRc01 | 2.66 ± 0.11 |
| HD 178484 | CoRoT LRc09 | 1.96 ± 0.07 |
| HD 181907 | CoRoT LRc01 | 2.35 ± 0.04 |
| HD 170053 | CoRoT LRc07, LRc08 | 1.85 ± 0.16 |
| HD 170174 | CoRoT LRc07, LRc08 | 2.56 ± 0.05 |
| HD 170231 | CoRoT LRc07, LRc08 | 2.74 ± 0.06 |
| α Boo | Coriolis satellite | 1.42 ± 0.08 |
| η Ser | Optical spectra | 3.00 ± 0.05 |
| ϵ Oph | MOST satellite | 2.64 ± 0.06 |
| ξ Hya | Optical spectra | 2.88 ± 0.05 |
| β Aql | Optical spectra | 3.53 ± 0.04 |
Notes. For the nomenclature of the CoRoT runs, SRa04 is, for instance, the fourth short run in the anticentre direction. Further details about the seismic data for the stars used for validation can be found in Tarrant et al. (2007; α Boo), Barban et al. (2004; η Ser), Kallinger et al. (2008; ϵ Oph), Frandsen et al. (2002; ξ Hya), and Kjeldsen et al. (2008; β Aql). For HD 45398, HD 49429, and HD 171427, the nature of the power spectrum hampered a robust determination of Δν and/or νmax. The seismic gravities are therefore not quoted in those cases.
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