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Table 5.

Metallicities, asteroseismic masses MAst. and evolutionary stages EAst. as determined by the reference given in the first column for 26 stars with asteroseismic as well as Bayesian stellar parameters and evolutionary stages available.

Ref. Source Identifier HIP [Fe/H] MAst. [M] EAst. Mtrk. [M] Etrk. Ptrk.
1 KIC 03730953 93687 −0.07 ± 0.03 1.97 ± 0.20a HB HB 0.996
1 KIC 04044238 94221 0.20 ± 0.03 1.06 ± 0.10a HB HB 0.824
1 KIC 05737655 98269 −0.63 ± 0.03 0.78 ± 0.08a HB RGB 0.683
1 KIC 08813946 95005 0.09 ± 0.03 2.09 ± 0.21a HB HB 0.997
1 KIC 09705687 94976 −0.20 ± 0.03 1.92 ± 0.19a HB HB 0.981
1 KIC 10323222 92885 0.04 ± 0.03 1.55 ± 0.16a RGB RGB 0.999
1 KIC 10404994 95687 −0.06 ± 0.03 1.50 ± 0.15a HB HB 0.990
1 KIC 10716853 93376 −0.08 ± 0.03 1.75 ± 0.18a HB HB 0.990
1 KIC 12884274 94896 0.11 ± 0.03 1.39 ± 0.14a HB HB 0.977
2 Tau 20889 0.17 ± 0.06b 2.40 ± 0.36 HB HB 0.993
2 β Gem 37826 0.09 ± 0.04b 1.73 ± 0.27 HB HB 0.994
2 18 Del 103527 0.07 ± 0.04c 1.92 ± 0.30 HB RGB 0.994
2 γ Cep 116727 0.13 ± 0.06 1.32 ± 0.20 RGB RGB 1.000
2 HD 5608 4552 0.12 ± 0.03 1.32 ± 0.21 RGB 1.574 ± 0.040 RGB 1.000
2 κ CrB 77655 0.13 ± 0.03 1.40 ± 0.21 RGB RGB 1.000
2 6 Lyn 31039 −0.13 ± 0.02 1.37 ± 0.22 RGB RGB 1.000
2 HD 210702 109577 0.04 ± 0.03 1.47 ± 0.23 RGB RGB 1.000
3 HD 145428 79364 −0.32 ± 0.12 RGB 1.000
3 HD 4313 3574 0.05 ± 0.1 RGB 1.000
3 HD 181342 95124 0.15 ± 0.1 1.380 ± 0.120 RGB 1.000
3 HD 5319 4297 0.02 ± 0.1 RGB 1.000
3 HD 185351 96459 0.00 ± 0.1b 1.77 ± 0.08 RGB 1.000
3 HD 212771 110813 −0.1 ± 0.12 1.46 ± 0.09 RGB 1.000
3 HD 106270 59625 0.06 ± 0.1 RGB 1.000
4 γ Piscium 114971 −0.54 ± 0.10b 1.00 ± 0.30d HBe HB 0.907
4 Θ1 Tauri 20885 0.08 ± 0.10b 2.70 ± 0.30 HBe HB 0.997

Notes. We also provide Bayesian masses Mtrk. and evolutionary stages EB. together with their probability Ptrk.

(a)

No confidence interval provided; we estimated a 10% error from Fig. 10 in Takeda & Tajitsu (2015).

(b)

Metallicity from Hekker & Meléndez (2007).

(c)

Metallicity from Maldonado et al. (2013).

(d)

No confidence interval provided; we assumed the same as for HIP 20885.

(e)

No mixed modes available, Beck et al. (2015) estimated the evolutionary stage from the frequency of the maximum oscillation power excess.

References. (1) Takeda & Tajitsu (2015); (2) Stello et al. (2017); (3) North et al. (2017); (4) Beck et al. (2015).

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