Table 3.
Radial velocity, atmospheric parameters, and abundances of the metal-poor RAVE stars in K2 Campaigns 1 and 3, as derived from RAVE spectra.
| ID | vrad | Teff | log(g) | [Fe/H] | [M/H] | [α/Fe] | [Mg/Fe] | [Si/Fe] | [Ti/Fe] |
|---|---|---|---|---|---|---|---|---|---|
| [km s−1] | [K] | [dex] | [dex] | [dex] | [dex] | [dex] | [dex] | [dex] | |
| S1 | 77.14 ± 0.85 | 5230 ± 62 | 2.24 ± 0.008 | −2.01 ± 0.10 | −1.92 ± 0.10 | 0.31 ± 0.13 | 0.54 ± 0.15 | 1.02 ± 0.17 | 1.29 ± 0.18 |
| S2 | −205.08 ± 0.87 | 5012 ± 81 | 2.58 ± 0.008 | −1.50 ± 0.09 | −1.29 ± 0.12 | 0.34 ± 0.16 | – | 0.54 ± 0.15 | – |
| S3 | 55.75 ± 0.69 | 4990 ± 93 | 2.57 ± 0.005 | −1.56 ± 0.10 | −1.24 ± 0.12 | 0.34 ± 0.15 | 0.76 ± 0.15 | 0.69 ± 0.15 | 1.11 ± 0.15 |
| S4 | −40.67 ± 1.45 | 5241 ± 90 | 3.17 ± 0.008 | −2.23 ± 0.12 | −2.23 ± 0.17 | 0.23 ± 0.18 | – | – | −0.05 ± 0.17 |
Notes. Temperature and abundances were derived by fixing the gravity to the seismic value (following the method described in Valentini et al. 2017) using RAVE spectra. Abundances were determined under LTE assumptions.
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