Table 1.
Physical parameters of the binaries.
| KIC | T2/T1 | (R2 + R1)/a | R2/R1 | Incl. | Ecc. | q | Porb [days] | Teff [K] |
|---|---|---|---|---|---|---|---|---|
| 10935310 | 0.650 ± 0.003 | 0.133 ± 0.0001 | 0.87 ± 0.003 | 84.33 ± 0.01 | 0.080 ± 0.0010 | 0.641 | 4.128795 | 5860 ± 30 |
| 5359678 | 0.914 ± 0.002 | 0.135 ± 0.0012 | 0.80 ± 0.044 | 85.39 ± 0.12 | 0.009 | 0.797 | 6.230610 | 6500 ± 30 |
| 8301013 | 0.967 ± 0.001 | 0.176 ± 0.0001 | 0.95 ± 0.012 | 87.93 ± 0.03 | 0.009 | 1.065 | 4.428059 | 6160 ± 20 |
| 3120320 | 0.624 ± 0.001 | 0.099 ± 0.0001 | 0.76 ± 0.007 | 86.20 ± 0.01 | 0.037 ± 0.0001 | 0.550 | 10.265613 | 5870 ± 30 |
| 8552540 | 0.881 ± 0.005 | 0.453 ± 0.0006 | 1.24 ± 0.015 | 84.72 ± 0.21 | 0.000 | 1.261 | 1.061934 | 6010 ± 40 |
| 9641031 | 0.833 ± 0.011 | 0.250 ± 0.0017 | 0.82 ± 0.041 | 85.77 ± 0.28 | 0.005 | 0.955 | 2.178154 | 6120 ± 60 |
| 10987439 | 1.363 ± 0.063 | 0.095 ± 0.0098 | 1.70 ± 0.028 | 85.28 ± 0.48 | 0.046 ± 0.0033 | – | 10.674599 | 6530 ± 100 |
| 11922782 | 0.864 ± 0.006 | 0.211 ± 0.0008 | 0.86 ± 0.037 | 83.84 ± 0.11 | 0.004 | 1.092 | 3.512934 | 5830 ± 20 |
| 6525196 | 0.967 ± 0.027 | 0.184 ± 0.0010 | 0.97 ± 0.203 | 84.02 ± 0.12 | 0.009 | 0.951 | 3.420604 | 6110 ± 20 |
| 4285087 | 0.989 ± 0.002 | 0.139 ± 0.0003 | 0.82 ± 0.024 | 87.16 ± 0.05 | 0.005 | 0.867 | 4.486031 | 5690 ± 30 |
| 6781535 | 0.960 ± 0.002 | 0.113 ± 0.0002 | 0.95 ± 0.014 | 84.44 ± 0.01 | 0.252 ± 0.0001 | – | 9.122086 | 5820 ± 60 |
| 7605600 | 0.812 ± 0.002 | 0.117 ± 0.0001 | 0.95 ± 0.004 | 85.72 ± 0.01 | 0.000 | 0.498 | 3.326193 | 3810 ± 30 |
| 8097825 | 0.912 ± 0.006 | 0.349 ± 0.0021 | 1.60 ± 0.030 | 78.24 ± 0.09 | 0.016 ± 0.0024 | 1.227 | 2.936852 | 5730 ± 30 |
| 6859813 | 0.557 ± 0.002 | 0.096 ± 0.0002 | 1.10 ± 0.016 | 85.78 ± 0.02 | 0.243 ± 0.0002 | – | 10.882422 | 6130 ± 10 |
| 5527172 | 0.529 ± 0.003 | 0.198 ± 0.0012 | 0.20 ± 0.001 | 83.13 ± 0.05 | 0.000 | 0.302 | 3.183967 | 5950 ± 30 |
| (318 rows) | ||||||||
Notes. (1) The eccentricity of near circular orbit is estimated with the Phoebe EBAI and LC geometry procedure. During the least-squares fitting procedure, this value was fixed because the least-squares method cannot learn more information about the eccentricity from the near circular orbit light curve. As a result, the eccentricity of a near circular orbit does not have an error estimate. Based on our trials, we adopted an eccentricity of 0.01 as the critical value to classify the orbit as near circular. (2) We do not provide errors of the mass ratio as it is too complex to estimate. (3) This table is available in full at the CDS.
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