Table 1.
Summary of the seismic and atmospheric properties for three rHB candidates of our sample (Sect. 2).
| KIC | L [L⊙] | Teff [K] | [Fe/H] | [α/Fe] | ⟨Δν⟩ [μHz] | νmax [μHz] | q | ΔΠ1 [s] | M [M⊙] |
|---|---|---|---|---|---|---|---|---|---|
| 5271626* | 42 ± 4 | 4769 ± 9 | 0.03 | 0.01 | 3.91 ± 0.05 | 25.1 ± 0.5 | 0.61 | 291.4 ± 1.7 | 0.66 ± 0.07 |
| 6032981+ | 44 ± 4 | 5300 ± 110 | −1.01 | 0.37 | 5.188 ± 0.017 | 35.4 ± 0.6 | 1.15 | 321 ± 3 | 0.68 ± 0.08 |
| 8694070 | 53 ± 5 | 5300 ± 30 | −1.44 | 0.25 | 5.135 ± 0.018 | 34.6 ± 0.6 | 0.7 | 332 ± 4 | 0.81 ± 0.09 |
| Mock rHB | 44 | 5663 | −1.00 | 0.2 | 6.41 | 42.5 | 0.65 | 324 | 0.65 |
| Mock RC | 59 | 4891 | 0.00 | 0.0 | 4.79 | 44.1 | 0.25 | 313 | 1.50 |
Notes. For each Kepler ID (KIC) we report: the effective temperature, Teff, the [Fe/H], and the [α/Fe] from APOGEE-DR17 or APOGEE-DR16 (one star marked with a plus sign); and the mean large frequency separation, ⟨Δν⟩, and frequency of maximum power, νmax, calculated by us using the code in Davies & Miglio (2016) or Yu et al. (2018) data (one star marked with an asterisk). The coupling factor, q, and asymptotic period spacing of the dipole modes, ΔΠ1, were calculated using the stretched-period method (see e.g., Vrard et al. 2016). The current stellar mass, M, was computed from Eq. (1). The last two rows show the properties of a simulated rHB and RC star (Sect. 3).
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