Table 5
Our measurements of candidate companions to CoRoT planet host stars.
| Target | MJD | N | Separation (′′) | Pos. angle (°) | Δr TCI | Δv TCI | Bound? | References |
|
|
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| CoRoT-2 | 56 778 | 2 | 4.061 ± 0.012 | 208.40 ± 0.15 | 2.901 ± 0.002 | – | – | 1, 5, 6, 7, 8 |
| CoRoT-3 (1) | 56 787 | 1 | 5.19 ± 0.02 | 174.7 ± 0.2 | 2.589 ± 0.004 | – | Yes (M) | 2, 6, 7, 8 |
| CoRoT-3 (2) | 56 787 | 1 | 4.96 ± 0.02 | 91.6 ± 0.2 | 4.8 ± 0.3 | – | – | 2, 7 |
| CoRoT-3 (3) | 56 787 | 1 | 2.501 ± 0.013 | 135.8 ± 0.2 | 6.295 ± 0.019 | – | – | – |
| CoRoT-3 (4) | 56 787 | 1 | 3.90 ± 0.03 | 240.7 ± 0.3 | 8.0 ± 0.6 | – | – | – |
| CoRoT-3 (5) | 56 787 | 1 | 4.51 ± 0.19 | 130.3 ± 0.2 | 7.6 ± 0.4 | – | – | – |
| CoRoT-4 (1) | 56 769 | 1 | 2.935 ± 0.014 | 336.8 ± 0.2 | 5.231 ± 0.014 | – | – | – |
| CoRoT-4 (2) | 56 769 | 1 | 4.187 ± 0.018 | 203.2 ± 0.2 | 6.9 ± 0.3 | – | – | – |
| CoRoT-6 | 56 785 | 2 | 4.620 ± 0.013 | 262.53 ± 0.15 | 6.63 ± 0.19 | – | – | – |
| CoRoT-7 | 56 769 | 1 | 4.98 ± 0.02 | 160.4 ± 0.2 | 8.9 ± 0.4 | – | No (B) | 3 |
| CoRoT-8 (1) | 56 840 | 4 | 2.468 ± 0.009 | 39.53 ± 0.12 | 7.174 ± 0.024 | Undetected | – | – |
| CoRoT-8 (2) | 56 840 | 4 | 3.163 ± 0.007 | 342.44 ± 0.11 | 6.468 ± 0.019 | Undetected | – | – |
| CoRoT-8 (3) | 56 840 | 4 | 4.290 ± 0.009 | 23.78 ± 0.11 | 6.236 ± 0.011 | 7.0 ± 0.6 | No (C) | – |
| CoRoT-9 (1) | 56 783 | 1 | 4.44 ± 0.02 | 271.2 ± 0.2 | 7.10 ± 0.05 | – | – | – |
| CoRoT-9 (2) | 56 783 | 1 | 4.618 ± 0.019 | 258.4 ± 0.2 | 5.185 ± 0.013 | – | – | – |
| CoRoT-11 (1) | 56 778 | 2 | 2.537 ± 0.009 | 307.01 ± 0.15 | 1.994 ± 0.002 | – | – | 4, 7, 8 |
| CoRoT-11 (2) | 56 778 | 2 | 3.043 ± 0.011 | 162.95 ± 0.15 | 7.228 ± 0.028 | – | – | – |
| CoRoT-11 (3) | 56 778 | 2 | 4.006 ± 0.014 | 222.27 ± 0.17 | 6.81 ± 0.18 | – | – | – |
Notes. “N” indicates the number of observations used for each star. Where more than one observation was used, the MJD quoted is in the middle of the range of observing dates. The “Bound?” column indicates cases where our analyses determined that the companion is bound or unbound, and the method with which this was confirmed (Proper Motion M, Relative Brightness B, or Stellar Colours C) – no entry is given if our analyses were inconclusive. The references column lists previous analyses (if any) of the candidates.
Reference. (1) Alonso et al. (2008); (2) Deleuil et al. (2008); (3) Léger et al. (2009); (4) Gandolfi et al. (2010); (5) Schröter et al. (2011); (6) Faedi et al. (2013); (7) Wöllert et al. (2015); (8) Wöllert & Brandner (2015).
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