Table 2.
Frequency of maximum amplitude νmax and large frequency separation Δν for the stars in the sample.
| KIC | νmax (μHz) | Δν (μHz) | Origin |
|---|---|---|---|
| 1430163 | 1805.07 ± 29.66 | 85.66 ± 1.80 | M14 |
| 1435467 | 1406.7 ± 8.4 | 70.369 ± 0.034 | L17 |
| 2837475 | 1557.6 ± 9.2 | 75.729 ± 0.042 | L17 |
| 3425851 | 2038 ± 60 | 92.6 ± 1.5 | H13 |
| 3456181 | 970.0 ± 8.3 | 52.264 ± 0.041 | L17 |
| 3733735 | 2132.61 ± 84.44 | 92.37 ± 1.72 | M14 |
| 4349452 | 2106 ± 50 | 98.27 ± 0.57 | H13 |
| 4638884 | 1192.28 ± 75.82 | 60.83 ± 1.15 | M14 |
| 5371516 | 1018.62 ± 59.84 | 55.46 ± 1.06 | M14 |
| 6225718 | 2364.2 ± 4.9 | 105.695 ± 0.018 | L17 |
| 6508366 | 958.3 ± 4.6 | 51.553 ± 0.047 | L17 |
| 6679371 | 941.8 ± 5.1 | 50.601 ± 0.029 | L17 |
| 7103006 | 1167.9 ± 7.2 | 59.658 ± 0.030 | L17 |
| 7206837 | 1652.5 ± 11.7 | 79.131 ± 0.039 | L17 |
| 7670943 | 1895 ± 73 | 88.6 ± 1.3 | H13 |
| 7771282 | 1465.1 ± 27.0 | 72.463 ± 0.079 | L17 |
| 7940546 | 1116.6 ± 3.6 | 58.762 ± 0.029 | L17 |
| 8179536 | 2074.9 ± 13.8 | 95.090 ± 0.058 | L17 |
| 8292840 | 1983 ± 37 | 92.85 ± 0.35 | H13 |
| 8694723 | 1470.5 ± 4.1 | 75.112 ± 0.021 | L17 |
| 8866102 | 2014 ± 32 | 94.50 ± 0.60 | H13 |
| 9139151 | 2690.4 ± 14.5 | 117.294 ± 0.032 | L17 |
| 9206432 | 1866.4 ± 14.9 | 84.926 ± 0.051 | L17 |
| 9226926 | 1411.43 ± 0.99 | 73.77 ± 1.26 | M14 |
| 9353712 | 934.3 ± 11.1 | 51.467 ± 0.104 | L17 |
| 9414417 | 1155 ± 32 | 60.05 ± 0.27 | H13 |
| 9812850 | 1255.2 ± 9.1 | 64.746 ± 0.068 | L17 |
| 10016239 | 2087.74 ± 22.83 | 101.60 ± 2.59 | M14 |
| 10355856 | 1298.44 ± 64.19 | 67.47 ± 1.43 | M14 |
| 11070918 | 1093.64 ± 20.03 | 66.89 ± 1.61 | M14 |
| 11081729 | 1968.3 ± 12.6 | 90.116 ± 0.048 | L17 |
| 11253226 | 1590.6 ± 10.6 | 76.858 ± 0.030 | L17 |
| 11807274 | 1496 ± 56 | 75.71 ± 0.31 | H13 |
| 12317678 | 1212.4 ± 5.5 | 63.464 ± 0.025 | L17 |
Notes. In the following order of priority for stars present in several lists, the seismic parameters are taken from Lund et al. (2017, L17), Mathur et al. (2014a, M14), and Huber et al. (2013, H13). For stars for which lower and upper uncertainties are provided, we retain only the largest value.
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