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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 (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; Jenkins et al., 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:
FileName Lrecl Records Explanations
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)
See also: V/133 : Kepler Input Catalog (Kepler Mission Team, 2009) Byte-by-byte Description of file: list.dat
Bytes Format Units Label Explanations
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)
Byte-by-byte Description of file: tablea.dat
Bytes Format Units Label Explanations
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)
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%.
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 19-Dec-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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