Table A.1
Spectroscopic parameters derived with ARES+MOOG.
| Star ID | T eff | log gspec | ξ t | [Fe/H] | N(Fe i, Fe ii) | σ(Fe i, Fe ii) | Transiting planet |
| [K] | [cm s-2] | [km s-1] | [dex] | [dex] | [Yes/No] | ||
|
|
|||||||
| 11 UMi | 4255 ± 88 | 1.80 ± 0.26 | 1.79 ± 0.08 | –0.13 ± 0.04 | 113, 15 | 0.18, 0.30 | No |
| 14 And | 4709 ± 37 | 2.44 ± 0.12 | 1.51 ± 0.03 | –0.29 ± 0.03 | 120, 15 | 0.09, 0.20 | No |
| 42 Dra | 4452 ± 42 | 2.09 ± 0.16 | 1.50 ± 0.04 | –0.41 ± 0.03 | 117, 15 | 0.10, 0.29 | No |
| 4 Uma | 4531 ± 52 | 2.32 ± 0.14 | 1.54 ± 0.04 | –0.19 ± 0.03 | 118, 15 | 0.11, 0.20 | No |
| 6 Lyn | 5022 ± 28 | 3.15 ± 0.13 | 1.16 ± 0.03 | –0.10 ± 0.02 | 118, 14 | 0.06, 0.23 | No |
| gam01 Leo | 4395 ± 48 | 1.66 ± 0.13 | 1.67 ± 0.04 | –0.47 ± 0.03 | 118, 15 | 0.12, 0.21 | No |
| HAT-P-14 | 6845 ± 108 | 4.62 ± 0.05 | 1.92 ± 0.15 | 0.17 ± 0.07 | 215, 34 | 0.19, 0.11 | Yes |
| HAT-P-22 | 5351 ± 57 | 4.22 ± 0.11 | 0.89 ± 0.10 | 0.28 ± 0.05 | 256, 33 | 0.13, 0.22 | Yes |
| HD 100655 | 4891 ± 46 | 2.79 ± 0.11 | 1.37 ± 0.04 | 0.07 ± 0.03 | 118, 15 | 0.10, 0.17 | No |
| HD 102956 | 5010 ± 37 | 3.31 ± 0.08 | 1.12 ± 0.04 | 0.12 ± 0.03 | 117, 15 | 0.08, 0.09 | No |
| HD 116029 | 4819 ± 54 | 2.98 ± 0.12 | 1.03 ± 0.06 | 0.09 ± 0.04 | 118, 15 | 0.11, 0.16 | No |
| HD 118203 | 5890 ± 41 | 4.10 ± 0.06 | 1.25 ± 0.04 | 0.30 ± 0.03 | 252, 33 | 0.10, 0.13 | No |
| (1) | 5910 ± 35 | 4.18 ± 0.07 | 1.34 ± 0.04 | 0.25 ± 0.03 | – | – | – |
| HD 131496 | 4886 ± 45 | 3.16 ± 0.11 | 1.16 ± 0.05 | 0.12 ± 0.03 | 119, 15 | 0.09, 0.15 | No |
| HD 132406 | 5766 ± 23 | 4.19 ± 0.03 | 1.05 ± 0.03 | 0.14 ± 0.02 | 253, 35 | 0.06, 0.06 | No |
| HD 132563B | 6073 ± 51 | 4.42 ± 0.05 | 1.02 ± 0.07 | –0.06 ± 0.04 | 246, 35 | 0.11, 0.11 | No |
| HD 136418 | 4979 ± 44 | 3.43 ± 0.08 | 1.03 ± 0.05 | –0.09 ± 0.03 | 118, 14 | 0.09, 0.08 | No |
| HD 139357 | 4595 ± 76 | 2.54 ± 0.20 | 1.61 ± 0.08 | 0.19 ± 0.05 | 117, 15 | 0.16, 0.31 | No |
| HD 145457 | 4829 ± 41 | 2.67 ± 0.10 | 1.48 ± 0.03 | –0.13 ± 0.03 | 119, 15 | 0.09, 0.16 | No |
| HD 152581 | 5095 ± 23 | 3.31 ± 0.05 | 1.07 ± 0.02 | –0.30 ± 0.02 | 119, 13 | 0.05, 0.07 | No |
| HD 154345 | 5442 ± 30 | 4.39 ± 0.04 | 0.76 ± 0.06 | –0.13 ± 0.02 | 256, 33 | 0.07, 0.10 | No |
| HD 158038 | 4822 ± 64 | 3.06 ± 0.16 | 1.11 ± 0.07 | 0.16 ± 0.05 | 119, 15 | 0.13, 0.23 | No |
| HD 16175 | 6022 ± 34 | 4.21 ± 0.06 | 1.26 ± 0.03 | 0.37 ± 0.03 | 255, 35 | 0.08, 0.13 | No |
| (1) | 6030 ± 22 | 4.23 ± 0.04 | 1.39 ± 0.02 | 0.32 ± 0.02 | – | – | – |
| HD 163607 | 5586 ± 29 | 4.05 ± 0.05 | 1.09 ± 0.03 | 0.22 ± 0.02 | 255, 35 | 0.07, 0.12 | No |
| HD 17092 | 4596 ± 65 | 2.45 ± 0.17 | 1.55 ± 0.06 | 0.05 ± 0.04 | 118, 15 | 0.14, 0.25 | No |
| HD 173416 | 4783 ± 43 | 2.43 ± 0.09 | 1.49 ± 0.03 | –0.15 ± 0.03 | 118, 14 | 0.10, 0.10 | No |
| HD 180314 | 4913 ± 60 | 2.90 ± 0.17 | 1.45 ± 0.05 | 0.11 ± 0.04 | 119, 15 | 0.13, 0.28 | No |
| HD 197037 | 6150 ± 34 | 4.37 ± 0.04 | 1.11 ± 0.04 | –0.16 ± 0.03 | 235, 36 | 0.08, 0.09 | No |
| HD 219415 | 4787 ± 53 | 3.22 ± 0.11 | 1.00 ± 0.06 | 0.03 ± 0.03 | 118, 14 | 0.10, 0.10 | No |
| HD 222155 | 5750 ± 23 | 4.00 ± 0.05 | 1.13 ± 0.02 | –0.09 ± 0.02 | 253, 34 | 0.06, 0.11 | No |
| (2) | 5765 ± 22 | 4.10 ± 0.13 | 1.22 ± 0.02 | –0.11 ± 0.05 | – | – | – |
| HD 240210 | 4316 ± 78 | 1.91 ± 0.21 | 1.76 ± 0.07 | –0.14 ± 0.03 | 115, 15 | 0.16, 0.26 | No |
| HD 240237 | 4422 ± 101 | 1.69 ± 0.24 | 2.31 ± 0.08 | –0.24 ± 0.06 | 111, 14 | 0.19, 0.30 | No |
| HD 32518 | 4661 ± 53 | 2.41 ± 0.12 | 1.53 ± 0.05 | –0.10 ± 0.04 | 119, 13 | 0.12, 0.16 | No |
| HD 96127 | 4179 ± 110 | 1.59 ± 0.34 | 2.01 ± 0.11 | –0.29 ± 0.05 | 114, 14 | 0.23, 0.40 | No |
| HD 99706 | 4891 ± 35 | 3.07 ± 0.08 | 1.15 ± 0.03 | 0.02 ± 0.03 | 119, 15 | 0.07, 0.12 | No |
| kappa CrB | 4889 ± 48 | 3.20 ± 0.11 | 1.13 ± 0.04 | 0.11 ± 0.03 | 120, 15 | 0.09, 0.14 | No |
| Kepler-21 | 6269 ± 47 | 4.07 ± 0.06 | 1.35 ± 0.05 | 0.03 ± 0.03 | 236, 34 | 0.10, 0.12 | Yes |
| omi CrB | 4792 ± 35 | 2.65 ± 0.14 | 1.48 ± 0.03 | –0.23 ± 0.03 | 119, 15 | 0.07, 0.25 | No |
Notes. log gspec is the spectroscopic surface gravity; ξt is the microturbulance speed; N(Fe i, Fe ii) is the number of lines used, and σ(Fe i, Fe ii) is the dispersion of the ion abundances in the spectroscopic analysis; (1) spectroscopic stellar parameters from SWEET-Cat derived in Santos et al. (2013); (2) spectroscopic stellar parameters from SWEET-Cat derived in Boisse et al. (2012).
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