J/A+A/543/A54 61 main-sequence and subgiant oscillations (Appourchaux+, 2012)
Oscillation mode frequencies of 61 main-sequence and subgiant stars observed
by Kepler.
Appourchaux T., Chaplin W.J., Garcia R.A., Gruberbauer M., Verner G.A.,
Antia H.M., Benomar O., Campante T.L., Davies G.R., Deheuvels S.,
Handberg R., Hekker S., Howe R., Regulo C., Salabert D., Bedding T.R.,
White T.R., Ballot J., Mathur S., Silva Aguirre V., Elsworth Y.P., Basu S.,
Gilliland R.L., Christensen-Dalsgaard J., Kjeldsen H., Uddin K.,
Stumpe M.C., Barclay T.
<Astron. Astrophys., 543, A54 (2012)>
=2012A&A...543A..54A 2012A&A...543A..54A (SIMBAD/NED BibCode)
ADC_Keywords: Asteroseismology ; Stars, dwarfs
Keywords: asteroseismology - stars: solar-type - stars: oscillations
Abstract:
Solar-like oscillations have been observed by Kepler and CoRoT in
several solar-type stars, thereby providing a way to probe the stars
using asteroseismology We provide the mode frequencies of the
oscillations of various stars required to perform a comparison with
those obtained from stellar modelling. We used a time series of nine
months of data for each star. The 61 stars observed were categorised
in three groups: simple, F-like, and mixed-mode. The simple group
includes stars for which the identification of the mode degree is
obvious. The F-like group includes stars for which the identification
of the degree is ambiguous. The mixed-mode group includes evolved
stars for which the modes do not follow the asymptotic relation of
low-degree frequencies. Following this categorisation, the power
spectra of the 61 main-sequence and subgiant stars were analysed using
both maximum likelihood estimators and Bayesian estimators, providing
individual mode characteristics such as frequencies, linewidths, and
mode heights. We developed and describe a methodology for extracting a
single set of mode frequencies from multiple sets derived by different
methods and individual scientists. We report on how one can assess the
quality of the fitted parameters using the likelihood ratio test and
the posterior probabilities. We provide the mode frequencies of 61
stars (with their 1-σ error bars), as well as their associated
echelle diagrams.
Description:
Kepler observations are obtained in two different operating modes:
long cadence (LC) and short cadence (SC) (Gilliland et al.,
2010ApJ...713L.160G 2010ApJ...713L.160G; Jenkins et al., 2010ApJ...713L..87J 2010ApJ...713L..87J). This work
is based on SC data. For the brightest stars (down to Kepler
magnitude, Kp~=12), SC observations can be obtained for a limited
number of stars (up to 512 at any given time) with a faster sampling
cadence of 58.84876s (Nyquist frequency of ∼8.5mHz), which permits a
more precise transit timing and the performance of asteroseismology.
Kepler observations are divided into three-month-long quarters (Q). A
subset of 61 solar-type stars observed during quarters Q5-Q7 (March
22, 2010 to December 22, 2010) were chosen because they have
oscillation modes with high signal-to-noise ratios. This length of
data gives a frequency resolution of about 0.04uHz.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 36 61 List of studied stars
tablea.dat 49 2599 Frequencies for 61 KIC (tables 3-7, A1-A56)
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [KIC]
5- 12 I8 --- KIC Star KIC number
14- 15 I2 h RAh Right ascension (J2000)
17- 18 I2 min RAm Right ascension (J2000)
20- 24 F5.2 s RAs Right ascension (J2000)
26 A1 --- DE- Declination sign (J2000)
27- 28 I2 deg DEd Declination (J2000)
30- 31 I2 arcmin DEm Declination (J2000)
33- 36 F4.1 arcsec DEs 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- 8 I8 --- KIC Star KIC number
10 I1 --- Degree [0/3] Degree
12- 19 F8.3 uHz Freq Frequency
21- 26 F6.3 uHz E_Freq ? 68% credible error (upper value)
27- 32 F6.3 uHz e_Freq ? 68% credible error (lower value) or
1σ error
34- 49 A16 --- Com Comments (1)
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Note (1): indication of the quality of the detection:
OK indicates that the mode was correctly detected and fitted;
Not detected indicates that the mode was fitted but not detected by the
quality assurance test and
Not fitted indicates that the mode was detected with a posterior probability
provided by the quality assurance test.
When an uncertainty and a posterior probability are quoted, it means that the
mode is fitted but detected using the quality assurance test with a
probability lower than 90%.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 19-Dec-2017