Table 2
Kepler objects of interest analyzed in this work.
| KOI | mKep | RA | Dec | Perioda | M⋆b | Rcompc | Nspec | Tspan |
| (mag) | (HH:MM:SS.SS) | (DD:MM:SS.SS) | (days) | (M⊙) | (R⊙) | (days) | ||
|
|
||||||||
| Group A − Eclipsing binaries | ||||||||
|
|
||||||||
| 340.01 | 13.1 | 19:50:39.52 | 47:48:05.01 | 23.673188 ± 0.000014 | 1.10 ± 0.07 | 0.231 ± 0.021† | 21 | 321.1 |
| 371.01 | 12.2 | 19:58:42.28 | 40:51:23.37 | 498.3928 ± 0.0042 | 1.55 ± 0.15 | 0.77 ± 0.39 | 29 | 722.0 |
| 686.01 | 13.6 | 19:47:21.78 | 43:38:49.64 | 52.513565 ± 0.000015 | 0.84 ± 0.12 | 0.1248 ± 0.0038‡ | 19 | 39.0 |
| 3725.01 | 10.1 | 19:40:48.69 | 38:31:10.38 | 1.5704970 ± 0.0000004 d | 2.52 ± 0.53 | 0.825 ± 0.007 | 10 | 17.0 |
| 3853.01 | 10.6 | 19:11:13.73 | 43:11:19.62 | 21.512905 ± 0.000050 | 1.55 ± 0.38 | 0.31 ± 0.22 | 25 | 70.9 |
|
|
||||||||
| Group B − Fast rotators | ||||||||
|
|
||||||||
| 12.01 | 11.4 | 19:49:48.90 | 41:00:39.56 | 17.855149 ± 0.000010 | 1.31 ± 0.27 | 0.122 ± 0.060 | 47 | 114.0 |
| 131.01 | 13.8 | 19:56:23.41 | 43:29:51.32 | 5.014233 ± 0.000002 | 1.31 ± 0.26 | 0.082 ± 0.029 | 29 | 418.0 |
| 366.01 | 11.7 | 19:26:39.40 | 38:37:09.32 | 75.11202 ± 0.00010 | 1.69 ± 0.17 | 0.097 ± 0.042 | 44 | 72.9 |
| 625.01 | 13.6 | 19:06:15.31 | 39:32:04.09 | 38.13819 ± 0.00021 | 1.46 ± 0.24 | 0.43 ± 0.21 | 52 | 66.0 |
| 972.01 | 9.3 | 18:48:00.07 | 48:32:32.00 | 13.118908 ± 0.000095 | 2.02 ± 0.07 | 0.055 ± 0.013 | 51 | 335.3 |
| 3728.01 | 12.3 | 19:35:05.31 | 44:38:18.49 | 5.5460830 ± 0.0000013 | 2.05 ± 0.17 | 0.1880 ± 0.0009 | 40 | 243.0 |
|
|
||||||||
| Group C − Unsolved cases | ||||||||
|
|
||||||||
| 1463.01 | 12.3 | 19:13:02.07 | 43:22:35.27 | 1064.2681410 ± 0.0001434 | 1.17 ± 0.28 | 0.149 | 14 | 691.2 |
| 3890.01 | 13.2 | 19:09:52.29 | 37:57:59.90 | 152.82630 ± 0.00099 | 1.76 ± 0.34 | 0.3213 ± 0.0091 | 22 | 305.2 |
Notes. Observational data obtained with CAFE at Calar Alto Observatory.
Transit periods are obtained from Borucki et al. (2011) and Batalha et al. (2013).
Stellar masses are obtained from Huber et al. (2014).
Radius of the transiting compnions according to Batalha et al. (2013).
This radius was obtained from our own transit fitting (see Sect. 4).
In this case, the radius of the companion was obtained from Díaz et al. (2014).
In Sect. 4, we have demonstrated that the actual period of this system is twice this value, i.e., 3.1409940 ± 0.0000008 days.
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