Table 10
Comparison between the improvements in the BSC parameter (in %) obtained by using the H11 (Howell et al. 2011), the A12 (Adams et al. 2012), and our high-resolution images (LB14) for all planet candidates involved (28 in H11 and 27 in A12).
| Planet | PBS,0 | PBS (%) | Planet | PBS,0 | PBS (%) | ||||
| candidate | % | H11 | A12 | LB14 | candidate | % | H11 | A12 | LB14 |
|
|
|||||||||
| 41.01 | 6.10 | 5.9 | 4.3 | 1.9 111.04 | 13.00 | 12.6 | 8.0 | 9.9 | |
| 41.02 | 10.10 | 9.9 | 8.2 | 5.8 | 115.01 | 4.50 | – | 2.5 | 1.9 |
| 41.03 | 9.40 | 9.2 | 7.6 | 5.2 | 115.02 | 7.40 | – | 5.4 | 4.8 |
| 49.01 | 8.10 | 7.4 | – | 3.4 | 115.03 | 14.80 | – | 12.8 | 12.2 |
| 69.01 | 4.10 | 4.0 | 2.0 | 1.5 | 196.01 | 4.00 | 2.8 | – | 0.4 |
| 82.01 | 1.30 | 1.2 | 0.4 | 0.2 | 245.01 | 0.90 | 0.9 | 0.3 | 0.1 |
| 82.02 | 2.50 | 2.4 | 1.5 | 1.0 | 245.02 | 2.30 | 2.3 | 1.7 | 1.3 |
| 82.03 | 3.10 | 3.0 | 2.1 | 1.6 | 245.03 | 5.30 | 5.3 | 4.7 | 4.2 |
| 82.04 | 4.20 | 4.1 | 3.2 | 2.7 | 245.04 | 4.10 | 4.1 | 3.5 | 3.1 |
| 82.05 | 5.30 | 5.2 | 4.3 | 3.8 | 366.01 | 2.40 | 2.0 | – | 0.7 |
| 94.01 | 3.70 | 3.1 | 0.9 | 0.3 | 372.01 | 4.20 | 3.4 | 0.2 | 0.8 |
| 94.02 | 10.60 | 10.0 | 6.5 | 4.1 | 398.01 | 3.80 | 2.5 | – | 0.9 |
| 94.03 | 6.80 | 6.2 | 2.7 | 1.2 | 398.02 | 8.50 | 7.2 | – | 5.4 |
| 94.04 | 23.80 | 23.2 | 19.7 | 17.2 | 398.03 | 13.50 | 12.2 | – | 10.4 |
| 111.01 | 5.40 | 5.1 | 0.9 | 2.3 | 638.01 | 15.20 | – | 3.2 | 8.8 |
| 111.02 | 5.60 | 5.3 | 1.0 | 2.6 | 638.02 | 14.60 | – | 2.7 | 8.3 |
| 111.03 | 4.90 | 4.6 | 0.7 | 1.9 | |||||
Notes. In all cases, the BSC has been improved with respect to the speckle images and the A12 study. Note that the common target KOI-0623 to H11 is not presented here because we detected a stellar companion closer than 3 arcsec. The small improvement of the H11 study is mostly due to the reduced field of view, which avoids detection of 1.5–3.0 arcsec companions, where the probability of having a background source is maximum in the 0–3 arcsec range.
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