Table 1.
Characteristics of Kepler red giants showing strongly distorted l = 1 doublets.
| KIC Id | M | Δν | ΔΠ1meas | z |
|---|---|---|---|---|
| (M⊙) | (μHz) | (s) | (s) | |
| 3326392 | 1.15 ± 0.05 | 10.64 ± 0.01 | 72.4 | −6.0 |
| 5700274 | 1.20 ± 0.07 | 11.89 ± 0.03 | 76.3 | −4.3 |
| 7458743 | 1.13 ± 0.07 | 10.89 ± 0.02 | 76.5 | −2.4 |
| 9227589 | 1.23 ± 0.06 | 15.25 ± 0.02 | 76.0 | −9.8 |
| 9697268 | 1.43 ± 0.09 | 11.38 ± 0.02 | 72.0 | −7.7 |
| 10613561 | 1.24 ± 0.08 | 14.76 ± 0.10 | 80.6 | −4.5 |
| 10976412 | 1.13 ± 0.07 | 11.58 ± 0.02 | 78.5 | −1.6 |
| 11408970 | 1.12 ± 0.07 | 13.85 ± 0.01 | 79.0 | −4.7 |
Notes. The columns give the KIC number of the stars in our catalog, the mass derived from seismic scaling relations (Yu et al. 2018), the average large separation of p modes Δν, the apparent period spacing of g modes ΔΠ1meas (see Sect. 2.2), and the distance from the degeneracy sequence z (see Sect. 2.3).
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