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J/ApJ/835/172 Kepler asteroseismic LEGACY sample. I. Oscillations (Lund+, 2017)

Standing on the shoulders of dwarfs: the Kepler asteroseismic LEGACY sample. I. Oscillation mode parameters. Lund M.N., Silva Aguirre V., Davies G.R., Chaplin W.J., Christensen-Dalsgaard J., Houdek G., White T.R., Bedding T.R., Ball W.H., Huber D., Antia H.M., Lebreton Y., Latham D.W., Handberg R., Verma K., Basu S., Casagrande L., Justesen A.B., Kjeldsen H., Mosumgaard J.R. <Astrophys. J., 835, 172-172 (2017)> =2017ApJ...835..172L (SIMBAD/NED BibCode)
ADC_Keywords: Stars, dwarfs Keywords: asteroseismology; stars: evolution; stars: fundamental parameters; stars: oscillations Abstract: The advent of space-based missions like Kepler has revolutionized the study of solar-type stars, particularly through the measurement and modeling of their resonant modes of oscillation. Here we analyze a sample of 66 Kepler main-sequence stars showing solar-like oscillations as part of the Kepler seismic LEGACY project. We use Kepler short-cadence data, of which each star has at least 12 months, to create frequency-power spectra optimized for asteroseismology. For each star, we identify its modes of oscillation and extract parameters such as frequency, amplitude, and line width using a Bayesian Markov chain Monte Carlo "peak-bagging" approach. We report the extracted mode parameters for all 66 stars, as well as derived quantities such as frequency difference ratios, the large and small separations Δν and δν02; the behavior of line widths with frequency and line widths at νmax with Teff, for which we derive parametrizations; and behavior of mode visibilities. These average properties can be applied in future peak-bagging exercises to better constrain the parameters of the stellar oscillation spectra. The frequencies and frequency ratios can tightly constrain the fundamental parameters of these solar-type stars, and mode line widths and amplitudes can test models of mode damping and excitation. Description: In erratum 2017, ApJ, 850, 110, we provide corrected sets of r01,10,02 difference ratio values and associated uncertainties, which were overestimated in the original paper (as noted by Roxburgh 2017A&A...604A..42R) due to a missing trimming in the post-processing of the Markov chain Monte Carlo (MCMC) chains for these values. We also provide updated values for the Δ2ν values of l=3 modes. See erratum for further explanations. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 139 66 Parameters for the targets in the studied sample table6.dat 96 2927 *Extracted mode parameters and quality control (Equations in section 3.2.3) for all sources including the Sun table7.dat 42 2541 *The calculated mode frequency difference ratios r01,10,02(n) (Equation 16) for all sources including the Sun table8.dat 41 2489 *Calculated second differences Δ2ν(n,l) (Equation 20) for all sources and the Sun
Note on table6.dat, table7.dat and table8.dat: From erratum published in 2017, ApJ, 850, 110
See also: V/133 : Kepler Input Catalog (Kepler Mission Team, 2009) J/A+A/508/L17 : Abundances in solar analogs (Ramirez+, 2009) J/A+A/510/A21 : Stellar Limb-Darkening Coefficients (Sing, 2010) J/A+A/531/A124 : Visibilities of stellar oscillation modes (Ballot+, 2011) J/A+A/529/A75 : Limb-darkening coefficients (Claret+, 2011) J/other/Nat/486.375 : Stellar parameters of KOI stars (Buchhave+, 2012) J/ApJS/199/30 : Effective temperatures for KIC stars (Pinsonneault+, 2012) J/ApJ/757/161 : Spectroscopy of 56 exoplanet host stars (Torres+, 2012) J/ApJ/767/127 : Asteroseismic solutions for 77 Kepler stars (Huber+, 2013) J/ApJ/787/110 : SAGA: Stromgren survey of seismic stars (Casagrande+, 2014) J/ApJS/210/1 : Asteroseismic study of solar-type stars (Chaplin+, 2014) J/A+A/569/A21 : Age and mass of CoRoT exoplanet host HD 52265 (Lebreton, 2014) J/ApJS/215/19 : APOKASC catalog of Kepler red giants (Pinsonneault+, 2014) J/MNRAS/452/2127 : Fundamental param. of Kepler stars (Silva Aguirre+, 2015) J/A+A/588/A87 : Seismic global parameters of 6111 KIC (Vrard+, 2016) J/ApJ/835/173 : Kepler asteroseismic LEGACY sample. II. (Silva Aguirre+, 2017) http://www.mso.anu.edu.au/saga/saga_home.html : SAGA home page Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 8 A8 --- KIC KIC number 10- 18 A9 --- Name Popular name 20- 24 F5.2 mag Kpmag [5.8/11] Kepler magnitude 26- 29 I4 uHz numax [885/4197] Frequency of maximum amplitude (νmax) (1) 31- 35 F5.1 uHz Dnu [48.4/173.5] Large frequency separation (Δν) (1) 37- 38 I2 --- N [22/59] Number of peak-bagged modes 40- 45 A6 --- Cat Category according to Appourchaux+ (2012A&A...543A..54A); "F-like" or "Simple" (44 occurrences) 47- 54 A8 --- BkQ Braketing quarters (2) 56- 73 A18 --- MgQ Missing quarters (2) 75- 78 I4 K Teff [5180/6642] Effective temperature (3) 80- 82 I3 K e_Teff [50/180] Teff uncertainty (4) 84 I1 --- r_Teff [1/6]? Reference for Teff (5) 86- 90 F5.2 [-] [Fe/H] [-1/0.4] Metallicity (3) 92- 95 F4.2 [-] e_[Fe/H] [0.02/0.2] [Fe/H] uncertainty (4) 97 I1 --- r_[Fe/H] [1/6]? Reference for [Fe/H] (5) 99-103 F5.3 [cm/s2] logg [3.9/4.6] Log surface gravity from Paper II (Silva Aguirre+, 2017, J/ApJ/835/173) 105-109 F5.3 [cm/s2] e_logg [0.002/0.02] Negative uncertainty on logg 111-115 F5.3 [cm/s2] E_logg [0.002/0.02] Positive uncertainty on logg 117-123 F7.2 km/s Vlos [-116/32]? Line-of-sight velocity (3) 125-128 F4.2 km/s e_Vlos [0.1]? Vlos uncertainty 130-134 F5.2 km/s vsini [0/24.1]? Rotational velocity (3) 136-139 F4.2 km/s e_vsini [0.5]? vsini uncertainty
Note (1): For uncertainties in νmax and Δν see Table 2. Note (2): First-last Kepler quarters during which the targets were observed in short-cadence (SC), and which quarters were missing in between. Note (3): Metallicities, temperatures, line of sight (LOS) velocities, and vsini values are adopted from the Stellar Parameters Classification tool (SPC; see Buchhave+ 2012, J/other/Nat/486.375) analysis of the targets unless otherwise indicated (see Note (5)). Note (4): Systematic uncertainties of ±59K (Teff) and ±0.062dex ([Fe/H]) have been added in quadrature as suggested by Torres+ (2012, J/ApJ/757/161). Note (5): Reference as follows: 1 = Pinsonneault et al. (2012, J/ApJS/199/30) 2 = Pinsonneault et al. (2014, J/ApJS/215/19) 3 = the SAGA project (Casagrande+ 2014, J/ApJ/787/110; see http://www.mso.anu.edu.au/saga/saga_home.html) 4 = Ramirez et al. (2009, J/A+A/508/L17) 5 = Chaplin et al. (2014, J/ApJS/210/1) 6 = Huber et al. (2013, J/ApJ/767/127)
Byte-by-byte Description of file: table6.dat
Bytes Format Units Label Explanations
1- 8 A8 --- KIC Kepler Input Catalog Identifier or "Sun" 10- 11 I2 --- n [8/31] Radial order 13 I1 --- l [0/3] Angular degree 15- 24 F10.5 uHz Freq [527.6/5729.7] Frequency 26- 32 F7.5 uHz e_Freq [0.03/6] Lower error on Freq 34- 40 F7.5 uHz E_Freq [0.03/6] Upper error on Freq 42- 48 F7.5 ppm Amp [0.05/6.5]? Amplitude 50- 56 F7.5 ppm e_Amp [0.02/0.8]? Lower error on Amp 58- 64 F7.5 ppm E_Amp [0.03/0.7]? Upper error on Amp 66- 73 F8.5 uHz Width [0.2/14.9]? Line width 75- 81 F7.5 uHz e_Width [0.04/4.3]? Lower error on Width 83- 89 F7.5 uHz E_Width [0.04/7.5]? Upper error on Width 91 A1 --- l_lnK Limit flag on lnK 92- 96 F5.2 [-] lnK [-1.4/6] Natural log of Bayes factor
Byte-by-byte Description of file: table7.dat
Bytes Format Units Label Explanations
1- 8 A8 --- KIC Kepler Input Catalog Identifier or "Sun" 10- 14 A5 --- Type Ratio type (r01, r02 or r10) (1) 16- 17 I2 --- n [10/30] Radial order 19- 26 F8.5 --- Ratio [-0.02/0.15] Mode frequency difference ratio 28- 34 F7.5 --- e_Ratio [0.0003/0.07] Lower error on Ratio 36- 42 F7.5 --- E_Ratio [0.0003/0.06] Upper error on Ratio
Note (1): Corresponding to the frequency ratios defined as (Roxburgh & Vorontsov 2003A&A...411..215R): r01(n)=d01(n)/Δν1(n), r10(n)=d10(n)/Δν0(n+1), r02(n)=(νn,0n-1,2)/Δν1(n) See Equation 16 in section 3.3.
Byte-by-byte Description of file: table8.dat
Bytes Format Units Label Explanations
1- 8 A8 --- KIC Kepler Input Catalog Identifier or "Sun" 10- 11 I2 --- n [9/30] Radial order 13 I1 --- l [0/3] Angular degree 15- 23 F9.5 uHz Del2nu [-11.4/12.1] Calculated 2nd difference Δ2ν (1) 25- 32 F8.5 uHz e_Del2nu [0.05/15.5] Lower error in Del2nu 34- 41 F8.5 uHz E_Del2nu [0.06/12.1] Upper error in Del2nu
Note (1): The second differences - Equation (20): Δ2ν(n,l)=νn-1,l-2νn,ln+1,l
History: From electronic version of the journal 15-Sep-2017: Insert into VizieR 27-Nov-2017: Tables 6, 7 and 8 updated from erratum published in 2017, ApJ, 850, 110. References: Silva Aguirre et al. Paper II. 2017ApJ...835..173S Cat. J/ApJ/835/173
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 18-Aug-2017
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