J/A+A/710/A369 6 seismic solar analogs asteroseismologic data (Garcia+, 2026)
Characterizing six seismic solar analogs observed by Kepler, K2, and HERMES.
Garcia R.A., Mathur S., Hookway G.T., Godoy-Rivera D., Masseron T.,
Betrisey J., Buldgen G., Lindsay C., Metcalfe T.S., Scutt O.J., Stokholm A.,
Beck P.G., Benomar O., Davies G.R., Jimenez A., Merc J., Nielsen M.B.,
Panetier E., Perez Hernandez F., Borg L., Breton S.N., Debacker L.,
Escorza A., Grossmann D.H., Hamy A., Liagre B., Lund M.N., Mathis S.,
Palakkatharappil D.B., Santos A.R.G., Delsanti V., Gonzalez-Cuesta L.,
Fox V., Proust N.
<Astron. Astrophys. 710, A369 (2026)>
=2026A&A...710A.369G 2026A&A...710A.369G (SIMBAD/NED BibCode)
ADC_Keywords: Stars, G-type ; Asteroseismology ; Optical
Keywords: stars: evolution - stars: oscillations - stars: solar-type
Abstract:
Solar analogs, stars that closely match the fundamental properties of
the Sun, provide key benchmarks for testing stellar structure and
evolution across different ages and activity levels. Their detailed
characterization helps place the Sun in context within the broader
population of solar-like stars. This study presents the
characterization of six seismic solar analogs observed by the NASA
Kepler and K2 missions. Combining asteroseismic constraints from
space-based photometry with high-resolution spectroscopy and Gaia
astrometry, we derived their fundamental parameters and assessed their
resemblance to the Sun. Global seismic properties and individual
oscillation modes were extracted from the photometric light curves,
while atmospheric parameters were obtained from data collected by the
HERMES spectrograph at the Mercator telescope. Stellar modeling using
seven independent stellar evolution codes yielded consistent masses,
radii, and ages. These stars have masses between 0.91 and
1.04M☉, radii between 0.95 and 1.08R☉, and ages from about
1.8 to 9.1Gyr, with typical systematic uncertainties of
±0.02M☉, ±0.01R☉, and ±0.7Gyr, respectively. One
star, EPIC 206064678, exhibits properties very similar to those of the
Sun, with M=1.016±0.033M☉, R=0.990±0.011R☉, and an age
of 5.40±0.12Gyr. It can therefore be considered a close solar twin,
although it is slightly older and more metal-rich (0.25±0.07dex).
Four targets display binarity signatures and all exhibit very low
chromospheric activity. This work broadens the sample of
well-characterized seismic solar analogs towards a larger sample of
metallicities and ages, providing new references for comparative
stellar studies and future asteroseismic investigations.
Description:
Frequencies and associated uncertainty for each detected modes (n, l),
and depending on the peakbagging code, for the full sample shown in
Appendix A.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
stars.dat 38 6 List of studied stars
tablea.dat 47 161 Frequencies and associated uncertainty for each
detected modes (n, l), and depending on the
peakbagging code, for the full sample shown
in Appendix A
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Byte-by-byte Description of file: stars.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Name KIC or EPIC identifier
16- 17 I2 h RAh Simbad right ascension (J2000)
19- 20 I2 min RAm Simbad right ascension (J2000)
22- 26 F5.2 s RAs Simbad right ascension (J2000)
28 A1 --- DE- Simbad declination sign (J2000)
29- 30 I2 deg DEd Simbad declination (J2000)
32- 33 I2 arcmin DEm Simbad declination (J2000)
35- 38 F4.1 arcsec DEs Simbad declination (J2000)
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Byte-by-byte Description of file: tablea.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Name KIC or EPIC identifier
16- 17 I2 --- n Radial order of the mode
19 I1 --- l Angular degree of the mode
21- 27 F7.2 uHz Freqapo ?=0 Mode frequency from Apollinaire (1)
29- 32 F4.2 uHz e_Freqapo ?=0 Uncertainty on apo_freq (1)
34- 40 F7.2 uHz Freqpbjam ?=0 Mode frequency from PBjam (1)
42- 45 F4.2 uHz e_Freqpbjam ?=0 Uncertainty on pbjam_freq (1)
47 I1 --- extended Mode quality flag (2)
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Note (1): Value set to 0.00 if not available
Note (2): Quality flag as follows:
0 = mode frequencies from both methods are consistent within 1 sigma
1 = mode frequencies from both methods are inconsistent within 1 sigma
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Acknowledgements:
Rafael Garcia, rgarcia(at)cea.fr
License: CC-BY-4.0
(End) Patricia Vannier [CDS] 24-Apr-2026