Table B.2
Compilation of the results from the spectroscopic analyses performed in the context of the spectroscopic follow-up of Kepler giant-planet candidates.
| KIC | KOI | Teff | log g | [Fe/H] | υsini⋆ | Method | References |
| [K] | [cm s-2] | [dex] | [km s-1] | ||||
|
|
|||||||
| 5812701 | 12 | 6800 ± 120 | 4.34 ± 0.15 | 0.09 ± 0.15 | 60.0 ± 1.5 | VWA | Bou15 |
| 9818381 | 135 | 6050 ± 100 | 4.40 ± 0.10 | 0.40 ± 0.10 | 5.5 ± 1.5 | MOOG | Bon15 |
| 5446285 | 142 | 5460 ± 70 | 4.60 ± 0.20 | 0.25 ± 0.09 | 2 ± 1 | VWA | Ba14 |
| 5357901 | 188 | 5170 ± 70 | 4.50 ± 0.15 | 0.24 ± 0.11 | 3 ± 1 | VWA | Hé14 |
| 11391018 | 189 | 4850 ± 100 | 4.60 ± 0.12 | –0.07 ± 0.12 | 2.5 ± 1.5 | VWA | Dí14 |
| 7950644 | 192 | 5800 ± 70 | 4.15 ± 0.15 | –0.19 ± 0.07 | 3 ± 1 | VWA | Hé14 |
| 11502867 | 195 | 5725 ± 90 | 4.50 ± 0.15 | –0.21 ± 0.08 | 3 ± 1 | VWA | Hé14 |
| 9410930 | 196 | 5750 ± 100 | 4.20 ± 0.10 | 0.38 ± 0.11 | 6 ± 2 | MOOG | Bon15 |
| 2987027 | 197 | 4995 ± 126 | 4.77 ± 0.30 | –0.11 ± 0.06 | 11 ± 1 | MOOG | Sa12 |
| 6046540 | 200 | 6000 ± 100 | 4.50 ± 0.10 | 0.42 ± 0.11 | 5 ± 1 | MOOG | Bon15 |
| 6849046 | 201 | 5526 ± 231 | 4.52 ± 0.40 | 0.28 ± 0.15 | 9 ± 1 | MOOG | Sa12 |
| 7877496 | 202 | 5750 ± 90 | 4.30 ± 0.07 | 0.27 ± 0.12 | 5 ± 1 | VWA | De14 |
| 9305831 | 204 | 5800 ± 100 | 4.10 ± 0.10 | 0.15 ± 0.10 | 4 ± 2 | MOOG | Bon15 |
| 7046804 | 205 | 5400 ± 75 | 4.70 ± 0.10 | 0.18 ± 0.12 | 2 ± 1 | MOOG | Bon15 |
| 5728139 | 206 | 6340 ± 140 | 4.00 ± 0.30 | 0.06 ± 0.19 | 11 ± 1 | VWA | Al15 |
| 10723750 | 209 | 6260 ± 80 | 4.40 ± 0.11 | 0.10 ± 0.13 | 6.8 ± 1 | VWA | Br15 |
| 6471021 | 372 | 5776 ± 46 | 4.12 ± 0.12 | –0.06 ± 0.04 | 4.1 ± 1.2 | MOOG | This work |
| 6289650 | 415 | 5810 ± 80 | 4.50 ± 0.20 | –0.24 ± 0.11 | 1.1 ± 1 | VWA | Mo13 |
| 9478990 | 423 | 6360 ± 100 | 4.40 ± 0.15 | 0.10 ± 0.14 | 16.0 ± 0.3 | MOOG | Bon15 |
| 10418224 | 428 | 6510 ± 100 | 4.10 ± 0.20 | 0.10 ± 0.15 | 9 ± 2 | VWA | Sa11 |
| 7368664 | 614 | 5970 ± 100 | 4.22 ± 0.10 | 0.35 ± 0.15 | 3 ± 1 | VWA | Al15 |
| 7529266 | 680 | 6090 ± 110 | 3.50 ± 0.10 | –0.17 ± 0.10 | 6 ± 1 | VWA | Al15 |
| 7906882 | 686 | 5750 ± 120 | 4.50 ± 0.15 | 0.02 ± 0.12 | 3.5 ± 1.0 | VWA | Dí14 |
| 5358624 | 830 | 5150 ± 100 | 5.00 ± 0.40 | 0.09 ± 0.17 | 2 ± 2 | VWA | Hé14 |
| 757450 | 889 | 5200 ± 100 | 4.60 ± 0.15 | 0.30 ± 0.12 | 3.5 ± 1.5 | MOOG | Bon15 |
| 3247268 | 1089 | 6027 ± 169 | 4.23 ± 0.29 | 0.31 ± 0.13 | 3.5 ± 1.2 | MOOG | This work |
| 8751933 | 1257 | 5520 ± 80 | 4.32 ± 0.10 | 0.27 ± 0.09 | 4 ± 2 | VWA | Sa14 |
| 8631160 | 1271 | 6600 ± 122 | 4.28 ± 0.23 | –0.06 ± 0.09 | 4.6 ± 1.2 | MOOG | This work |
| 7303287 | 1353 | 6326 ± 126 | 4.50 ± 0.25 | 0.33 ± 0.09 | 5.3 ± 1.2 | MOOG | This work |
| 9425139 | 1411 | 5687 ± 146 | 4.32 ± 0.29 | 0.47 ± 0.12 | 4.6 ± 1.2 | MOOG | This work |
| 11075279 | 1431 | 5507 ± 74 | 4.36 ± 0.25 | 0.27 ± 0.05 | 4.6 ± 1.2 | MOOG | This work |
| 10005758 | 1783 | 6298 ± 150 | 4.30 ± 0.30 | 0.49 ± 0.12 | 3.0 ± 1.2 | MOOG | This work |
| 2975770 | 1788 | 4890 ± 232 | 4.58 ± 0.59 | 0.05 ± 0.39 | 6.2 ± 1.2 | MOOG | This work |
| 12735740 | 3663 | 5649 ± 162 | 4.27 ± 0.34 | 0.14 ± 0.12 | 3.4 ± 1.2 | MOOG | This work |
| 10795103 | 3683 | 6666 ± 203 | 4.39 ± 0.30 | 0.24 ± 0.16 | 8.9 ± 1.2 | MOOG | This work |
| 7017372 | 3689 | 6154 ± 253 | 4.51 ± 0.36 | 0.31 ± 0.21 | 2.4 ± 1.2 | MOOG | This work |
| 12645761 | 5976 | 4753 ± 90 | 2.87 ± 0.29 | 0.01 ± 0.06 | 4.8 ± 1.2 | MOOG | This work |
Notes. The instrumental resolution of SOPHIE corresponds to a υsini⋆ of ~4 km s-1 for a solar-like star. Therefore, υsini⋆ vales lower than 4 km s-1 should be considered as upper limits.
Reference. Al15: Almenara et al. (2015); Ba14: Barros et al. (2014); Bon15: Bonomo et al. (2015); Bou15: Bourrier et al. (2015); Br15: Bruno et al. (2015); De14: Deleuil et al. (2014); Dí14: Díaz et al. (2014b); Hé14: Hébrard et al. (2014); Mo13: Moutou et al. (2013a); Sa11: Santerne et al. (2011a); Sa12: Santerne et al. (2012b); Sa14: Santerne et al. (2014).
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