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Table 3

Photospheric and chromospheric activity properties of the 18 seismic solar analogs derived from the photometric Kepler and spectroscopic Hermes observations.

# Star KIC Prot (days) Sph (ppm) index log S/N(Ca) ΔT (days) N spec

1 3241581 26.3 ± 2.0 236.9 ± 3.8 0.182 ± 0.024 − 4.868 ± 0.164 17.1 504 23
2 3656476 31.7 ± 3.5 89.1 ± 1.6 0.168 − 5.002 ± 0.100 24.5 <1 1
3 4914923 20.5 ± 2.8 139.1 ± 2.5 0.168 ± 0.014 − 4.918 ± 0.100 26.6 34 6
4 5084157 22.2 ± 2.8 270.8 ± 4.8 0.217 ± 0.107 − 4.840 ± 0.580 11.0 33 9
5 5774694 12.1 ± 1.0 2492.3 ± 61.2 0.269 ± 0.021 − 4.581 ± 0.059 23.7 36 3
6 6116048 17.3 ± 2.0 90.2 ± 1.9 0.157 ± 0.001 − 4.984 ± 0.042 24.1 35 3
7 6593461 25.7 ± 3.0 188.8 ± 3.6 0.260 ± 0.119 − 4.550 ± 0.333 10.4 35 8
8 7296438 25.2 ± 2.8 177.1 ± 3.0 0.162 − 4.994 ± 0.151 20.4 35 3a
9 7680114 26.3 ± 1.9 50.2 ± 1.0 0.185 ± 0.019 − 4.881 ± 0.164 19.4 35 3
10 7700968 36.2 ± 4.2 88.9 ± 1.4 0.181 ± 0.010 − 4.866 ± 0.123 19.8 35 3
11 9049593 12.4 ± 2.5 290.8 ± 6.4 0.177 ± 0.016 − 4.955 ± 0.200 18.4 35 3
12 9098294 19.8 ± 1.3 292.7 ± 5.2 0.203 ± 0.031 − 4.737 ± 0.136 19.5 35 3
13 10130724 32.6 ± 3.0 155.0 ± 2.5 0.252 ± 0.067 − 4.548 ± 0.246 10.6 34 5
14 10215584 22.2 ± 2.9 138.3 ± 2.5 0.215 ± 0.049 − 4.738 ± 0.211 17.4 35 4
15 10644253 10.9 ± 0.9 549.4 ± 13.3 0.219 ± 0.014 − 4.691 ± 0.059 30.1 180 12
16 10971974 26.9 ± 4.0 309.9 ± 4.9 0.241 ± 0.066 − 4.761 ± 0.312 10.0 35 3
17 11127479 17.6 ± 1.8 115.9 ± 2.8 0.271 ± 0.169 − 4.683 ± 0.482 10.2 35 4
18 11971746 19.5 ± 2.1 90.5 ± 2.0 0.152 ± 0.028 − 4.937 ± 0.217 16.6 34 7

Notes. The surface rotation periods, Prot, were measured by García et al. (2014) from the Kepler observations. The columns ΔT and Nspec corresponds respectively to the interval of time covered by the Hermes observations and the associated number of analyzed spectra. The two stars indicated by the symbol () a re candidates for hosting a planetary system from the Kepler Objects of Interest (KOI) list (source: MAST at https://archive.stsci.edu/kepler/).

(a)

In the case of KIC 7296438, three Hermes spectra were collected, but only one spectrum has a signal-to-noise (S/N) high enough to measure the index.

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