J/ApJS/210/1 Asteroseismic study of solar-type stars (Chaplin+, 2014)
Asteroseismic fundamental properties of solar-type stars observed by the NASA
Kepler mission.
Chaplin W.J., Basu S., Huber D., Serenelli A., Casagrande L.,
Silva Aguirre V., Ball W.H., Creevey O.L., Gizon L., Handberg R.,
Karoff C., Lutz R., Marques J.P., Miglio A., Stello D., Suran M.D.,
Pricopi D., Metcalfe T.S., Monteiro M.J.P.F.G., Molenda-Zakowicz J.,
Appourchaux T., Christensen-Dalsgaard J., Elsworth Y., Garcia R.A.,
Houdek G., Kjeldsen H., Bonanno A., Campante T.L., Corsaro E., Gaulme P.,
Hekker S., Mathur S., Mosser B., Regulo C., Salabert D.
<Astrophys. J. Suppl. Ser., 210, 1 (2014)>
=2014ApJS..210....1C 2014ApJS..210....1C (SIMBAD/NED BibCode)
ADC_Keywords: Abundances, [Fe/H] ; Effective temperatures ; Stars, masses ;
Stars, ages
Keywords: asteroseismology - methods: data analysis -
stars: fundamental parameters - stars: interiors
Abstract:
We use asteroseismic data obtained by the NASA Kepler mission to
estimate the fundamental properties of more than 500 main-sequence and
sub-giant stars. Data obtained during the first 10 months of Kepler
science operations were used for this work, when these solar-type
targets were observed for one month each in survey mode. Stellar
properties have been estimated using two global asteroseismic
parameters and complementary photometric and spectroscopic data.
Homogeneous sets of effective temperatures, Teff, were available for
the entire ensemble from complementary photometry; spectroscopic
estimates of Teff and [Fe/H] were available from a homogeneous
analysis of ground-based data on a subset of 87 stars. We adopt a
grid-based analysis, coupling six pipeline codes to 11 stellar
evolutionary grids. Through use of these different grid-pipeline
combinations we allow implicitly for the impact on the results of
stellar model dependencies from commonly used grids, and differences
in adopted pipeline methodologies. By using just two global parameters
as the seismic inputs we are able to perform a homogeneous analysis of
all solar-type stars in the asteroseismic cohort, including many
targets for which it would not be possible to provide robust estimates
of individual oscillation frequencies (due to a combination of low
signal-to-noise ratio and short dataset lengths). The median final
quoted uncertainties from consolidation of the grid-based analyses are
for the full ensemble (spectroscopic subset) approximately 10.8%
(5.4%) in mass, 4.4% (2.2%) in radius, 0.017 dex (0.010 dex) in log g,
and 4.3% (2.8%) in mean density. Around 36% (57%) of the stars have
final age uncertainties smaller than 1 Gyr. These ages will be useful
for ensemble studies, but should be treated carefully on a
star-by-star basis. Future analyses using individual oscillation
frequencies will offer significant improvements on up to 150 stars, in
particular for estimates of the ages, where having the individual
frequency data is most important.
Description:
During the first 10 months of science operations more than 2000
solar-type stars were selected by the Kepler Asteroseismic Science
Consortium (KASC) to be observed as part of an asteroseismic survey of
the Sun-like population in the Kepler field of view. Solar-like
oscillations were detected by Kepler in more than 500 stars (Chaplin
et al. 2011Sci...332..213C 2011Sci...332..213C), and from these data robust global or
average asteroseismic parameters were determined for all targets in
the sample. These asteroseismic parameters allow us to estimate
fundamental properties of the stars. In this paper we present stellar
properties - namely masses, radii, surface gravities, mean densities
and ages - of this asteroseismic sample of main-sequence and subgiant
stars.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 56 518 *Seismic and non-seismic input parameters for the
full cohort, with photometric SDSS-calibrated
and IRFM Teff and field-average [Fe/H]
table2.dat 46 87 Seismic and non-seismic input parameters for the
sample with spectroscopic Teff and [Fe/H]
from Bruntt et al. (2012, Cat. J/MNRAS/423/122)
table4.dat 91 518 *Estimated stellar properties using SDSS-calibrated
Teff and field-average [Fe/H] values
table5.dat 91 518 *Estimated stellar properties using IRFM Teff
and field-average [Fe/H] values
table6.dat 91 87 Estimated stellar properties using spectroscopic
Teff and [Fe/H] values from Bruntt et al.
(2012, Cat. J/MNRAS/423/122)
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Note on table1.dat, table4.dat, table5.dat: One set of temperatures was derived
by using an Infra-Red Flux Method (IRFM) calibration (Casagrande et al. 2010,
Cat. J/A+A/512/A54; see also Silva Aguirre et al. 2012ApJ...757...99S 2012ApJ...757...99S). This
made use of multi-band JHK photometry from the Two Micron All Sky Survey
(Skrutskie et al. 2006, Cat. II/246), photometry in the Sloan Digital Sky
Survey (SDSS) griz bands available in the KIC, and reddening estimates from
Drimmel et al. (2003A&A...409..205D 2003A&A...409..205D).
A second set of temperatures were those derived by Pinsonneault et al. (2012,
Cat. J/ApJS/199/30), who performed a recalibration of the KIC photometry in
the SDSS griz filters, using YREC models.
See section 3 for further explanations.
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/ApJS/199/30 : Eff. temperature scale for KIC stars (Pinsonneault+, 2012)
J/MNRAS/423/122 : Abundances of 93 solar-type Kepler targets (Bruntt+, 2012)
J/A+A/547/A36 : Chemical abundances of 87 KOIs (Adibekyan++, 2012)
J/ApJ/749/152 : Asteroseismic analysis of 22 solar-type stars (Mathur+, 2012)
J/A+A/534/A125 : Var. of A- and F-stars from Kepler (Uytterhoeven+ 2011)
J/MNRAS/412/1210 : Kepler asteroseismic targets (Molenda-Zakowicz+, 2011)
J/ApJ/729/L10 : KIC stars properties in NGC 6791 and NGC 6819 (Basu+, 2011)
J/A+A/517/A3 : Kepler early-type targets stellar param. (Catanzaro+, 2010)
J/ApJ/718/L97 : Early asteroseismic results from Kepler (Van Grootel+, 2010)
J/A+A/512/A54 : Teff and Fbol from Infrared Flux Method (Casagrande+, 2010)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 I8 --- KIC Kepler identifier (Cat. V/133)
10- 13 I4 uHz numax [250/3481]? Frequency of maximum oscillations
power
15- 17 I3 uHz e_numax ? Uncertainty in numax
19- 23 F5.1 uHz Dnu [17/174] Average large frequency separation
25- 27 F3.1 uHz e_Dnu Uncertainty in Dnu
29- 32 I4 K T(SDSS) [4814/7149]? SDSS derived effective temperature
34- 36 I3 K e_T(SDSS) ? Uncertainty in T(SDSS)
38- 41 I4 K T(IRFM) [4801/7066]? IR Flux Method derived effective
temperature
43- 45 I3 K e_T(IRFM) ? Uncertainty in T(IRFM)
47- 51 F5.2 [-] [Fe/H] [-0.2] Field-averaged metallicity
53- 56 F4.2 [-] e_[Fe/H] [0.3] Uncertainty in [Fe/H]
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 I8 --- KIC Kepler identifier
10- 13 I4 uHz numax [277/3481]? Frequency of maximum oscillations
power
15- 17 I3 uHz e_numax ? Uncertainty in numax
19- 23 F5.1 uHz Dnu [20/154] Average large frequency separation
25- 27 F3.1 uHz e_Dnu Uncertainty in Dnu
29- 32 I4 K Teff [5094/6892] Effective temperature
34- 35 I2 K e_Teff Uncertainty in Teff
37- 41 F5.2 [-] [Fe/H] [-1.2/0.5] Metallicity; [Fe/H]
43- 46 F4.2 [-] e_[Fe/H] [0.09] Uncertainty in [Fe/H]
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Byte-by-byte Description of file: table[456].dat
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Bytes Format Units Label Explanations
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1- 8 I8 --- KIC Kelper identifier
10- 13 F4.2 Msun Mass [0.8/2]? Mass
15- 18 F4.2 Msun E_Mass ? Upper uncertainty in Mass
20- 23 F4.2 Msun e_Mass ? Lower uncertainty in Mass
25- 28 F4.2 Rsun Rad [0.8/5]? Radius
30- 33 F4.2 Rsun E_Rad ? Upper uncertainty in Rad
35- 38 F4.2 Rsun e_Rad ? Lower uncertainty in Rad
40- 45 F6.4 [Sun] rho [0.01/1.7]? Density relative to ρ☉
47- 52 F6.4 [Sun] E_rho ? Upper uncertainty in rho
54- 59 F6.4 [Sun] e_rho ? Lower uncertainty in rho
61- 65 F5.3 [cm/s2] log(g) [3.3/4.6]? Log of surface gravity
67- 71 F5.3 [cm/s2] E_log(g) ? Upper uncertainty in log(g)
73- 77 F5.3 [cm/s2] e_log(g) ? Lower uncertainty in log(g)
79- 82 F4.1 Gyr Age [0.3/14]? Age
84- 87 F4.1 Gyr E_Age ? Upper uncertainty in Age
89- 91 F3.1 Gyr e_Age ? Lower uncertainty in Age
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 27-Jan-2014