Table E.1.
Ages and masses of the four RAVE stars as derived by PARAM, using COR seismic pipeline and stellar parameters obtained from different spectra, RAVE, and ESO-UVES (after adopting the strategy of using seismic gravities to find a more self-consistent surface temperature).
| Star | Seismic | RAVE | UVES | UVES+Gaia | |||
|---|---|---|---|---|---|---|---|
| ID | pipeline | Age | Mass | Age | Mass | Age | Mass |
| [Gyr] | [M⊙] | [Gyr] | [M⊙] | [Gyr] | [M⊙] | ||
| S1 | COR |  |
 |
 |
 |
 |
 |
| COR2σTeff |  |
 |
|||||
| CORage lim. |  |
 |
 |
 |
|||
| BM_N |  |
 |
|||||
| S2 | COR |  |
 |
 |
 |
 |
 |
| COR2σTeff |  |
 |
|||||
| CORage lim. |  |
 |
 |
 |
|||
| BM_N |  |
 |
|||||
| S3 | COR |  |
 |
 |
 |
 |
 |
| COR2σTeff | – | – |  |
 |
|||
| CORage lim. |  |
 |
 |
 |
|||
| BM_N |  |
 |
|||||
| S4 | COR |  |
 |
 |
 |
 |
 |
| COR2σTeff | – | – |  |
 |
|||
| CORage lim. |  |
 |
 |
 |
|||
| BM_N |  |
 |
|||||
Notes. For the PARAM results obtained from RAVE spectra, we listed the values corresponding to an α enhancement closer to that measured. Maximum and minimum error values of age and mass (measured on the 68 percentile of the PDF) are listed in superscript and subscript, respectively. The COR2σTeff and CORage lim. rows list the mass and age determined by doubling the error on Teff and adding the upper limit on age (13.96 Gyr), respectively.
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