Fundamental properties of five Kepler stars using global asteroseismic quantities and ground-based observations

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Volume 537 (January 2012)

A&A, 537 (2012) A111

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Table A.1

Published frequencies given in μHz for stars KIC 11395018 (C1), KIC 10273246 (C2), KIC 10920273 (C3), and KIC 11234888 (C5), as reported by Campante et al. (2011) and Mathur et al. (2011).

KIC 11395018

KIC 10273246

KIC 10920273

KIC 11234888

686.66 ± 0.32

737.90 ± 0.30

826.66^a ± 0.25

627.67 ± 0.19

732.37 ± 0.18

785.40 ± 0.20

882.77 ± 0.20

669.35 ± 0.16

779.54 ± 0.14

833.90 ± 0.20

939.58 ± 0.16

711.63 ± 0.15

827.55 ± 0.15

883.50 ± 0.20

997.14 ± 0.18

753.64 ± 0.20

875.40 ± 0.16

932.70 ± 0.50

1054.33 ± 0.30

794.56 ± 0.20

923.16 ± 0.19

981.10 ± 0.30

1111.51 ± 0.25

836.83 ± 0.21

971.05 ± 0.28

1030.70 ± 0.40

1170.77^a ± 0.33

877.80^a ± 0.22

...

1079.30 ± 0.20

1226.34^a ± 0.33

...

667.05^a ± 0.22

622.80 ± 0.20

794.65^b ± 0.32

506.72 ± 0.20

707.66 ± 0.19

661.90 ± 0.50

838.61^b ± 0.25

563.30 ± 0.14

740.29^b ± 0.17

695.75^b ± 0.27

914.52 ± 0.16

594.83 ± 0.16

763.99 ± 0.18

724.70 ± 0.20

968.19 ± 0.13

686.34 ± 0.17

805.74 ± 0.13

764.30 ± 0.30

1023.58 ± 0.14

741.10 ± 0.18

851.37 ± 0.11

809.80 ± 0.20

1079.10 ± 0.31

815.43 ± 0.21

897.50 ± 0.15

857.30 ± 0.20

1135.36^c ± 0.31

855.67 ± 0.21

940.50 ± 0.15

905.60 ± 0.30

...

997.91 ± 0.33

950.00 ± 0.30

...

1008.60 ± 0.40

...

1056.30 ± 0.20

...

1103.30 ± 0.40

...

631.19^a ± 1.36

688.50 ± 0.70

822.39^a ± 0.28

582.84^a ± 0.21

680.88 ± 0.45

734.80 ± 0.60

873.10^a^d ± 0.32

624.65 ± 0.18

727.78 ± 0.30

779.50 ± 0.40

934.49 ± 0.22

708.67 ± 0.19

774.92 ± 0.16

830.30 ± 0.40

992.44 ± 0.13

751.84 ± 0.21

823.50 ± 0.16

880.60 ± 0.50

1049.36 ± 0.39

...

871.29 ± 0.21

927.50 ± 0.40

1106.76 ± 0.34

...

918.10 ± 0.28

977.60 ± 0.40

...

965.83 ± 0.23

1025.30 ± 1.30

...

1016.61^e^f ± 0.73

1073.70 ± 0.20

...

1122.70^a^d ± 0.40

...

Notes. The frequencies were fitted with 11, 10, 10, and 11 different methods, and a criteria was imposed to obtain a minimal frequency set representative of the results from most of the fitters.

^(a)

Frequencies not among the minimal set.

^(b)

l = 1 mixed mode.

^(c)

Mode close to the second harmonic of the inverse of the long-cadence period.

^(d)

Possible l = 2 mixed mode introduced a posteriori.

^(e)

Uncertain identification.

^(f)

Mode tagging changed a posteriori from l = 0 to l = 2.

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