J/MNRAS/452/2127 Fundamental parameters of Kepler stars (Silva Aguirre+, 2015)
Ages and fundamental properties of Kepler exoplanet host stars from
asteroseismology.
Silva Aguirre V., Davies G.R., Basu S., Christensen-dalsgaard J.,
Creevey O., Metcalfe T.S., Bedding T.R., Casagrande L., Handberg R.,
Lund M.N., Nissen P.E., Chaplin W.J., Huber D., Serenelli A.M., Stello D.,
Van Eylen V., Campante T.L., Elsworth Y., Gilliland R.L., Hekker S.,
Karoff C., Kawaler S.D., Kjeldsen H., Lundkvist M.S.
<Mon. Not. R. Astron. Soc., 452, 2127-2148 (2015)>
=2015MNRAS.452.2127S 2015MNRAS.452.2127S (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets ; Stars, masses
Keywords: asteroseismology - planets and satellites: fundamental parameters -
stars: evolution - stars: fundamental parameters -
stars: oscillations - planetary systems
Abstract:
We present a study of 33 Kepler planet-candidate host stars for which
asteroseismic observations have sufficiently high signal-to-noise
ratio to allow extraction of individual pulsation frequencies. We
implement a new Bayesian scheme that is flexible in its input to
process individual oscillation frequencies, combinations of them, and
average asteroseismic parameters, and derive robust fundamental
properties for these targets. Applying this scheme to grids of
evolutionary models yields stellar properties with median statistical
uncertainties of 1.2 per cent (radius), 1.7 per cent (density), 3.3
per cent (mass), 4.4 per cent (distance), and 14 per cent (age),
making this the exoplanet host-star sample with the most precise and
uniformly determined fundamental parameters to date. We assess the
systematics from changes in the solar abundances and mixing-length
parameter, showing that they are smaller than the statistical errors.
We also determine the stellar properties with three other fitting
algorithms and explore the systematics arising from using different
evolution and pulsation codes, resulting in 1 per cent in density and
radius, and 2 per cent and 7 per cent in mass and age, respectively.
We confirm previous findings of the initial helium abundance being a
source of systematics comparable to our statistical uncertainties, and
discuss future prospects for constraining this parameter by combining
asteroseismology and data from space missions. Finally, we compare our
derived properties with those obtained using the global average
asteroseismic observables along with effective temperature and
metallicity, finding excellent level of agreement. Owing to selection
effects, our results show that the majority of the high
signal-to-noise ratio asteroseismic Kepler host stars are older than
the Sun.
Description:
Our sample has been extracted from the 77 exoplanet host stars
presented in Huber et al. (2013, Cat. J/ApJ/767/127).
We have made use of the full time-base of observations from the Kepler
satellite to uniformly determine precise fundamental stellar
parameters, including ages, for a sample of exoplanet host stars where
high-quality asteroseismic data were available. We devised a Bayesian
procedure flexible in its input and applied it to different grids of
models to study systematics from input physics and extract
statistically robust properties for all stars.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 260 33 Recommended set of stellar properties and
statistical uncertainties of exoplanet
candidate host stars as determined with BASTA
tablea1.dat 86 33 Stellar properties determined with ASTFIT
tablea2.dat 112 29 Stellar properties determined with YMCM
tablea3.dat 122 34 Stellar properties determined with AMP
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/ApJ/767/127 : Asteroseismic solutions for 77 Kepler stars (Huber+, 2013)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- KOI KOI number
6- 13 I8 --- KIC KIC number
15- 18 I4 K Teff Effective temperature
20- 22 I3 K e_Teff rms uncertainty on Teff (1)
24- 28 F5.2 [-] [Fe/H] Metallicity
30- 33 F4.2 [-] e_[Fe/H] rms uncertainty on [Fe/H] (1)
35- 39 F5.3 Msun Mass Mass
41- 45 F5.3 Msun E_Mass rms uncertainty on Mass (1)
47- 51 F5.3 Msun e_Mass Radius (1)
53- 57 F5.3 Rsun Radius rms uncertainty on Radius
59- 63 F5.3 Rsun E_Radius Error on radius (upper value) (1)
65- 69 F5.3 Rsun e_Radius Error on radius (lower value) (1)
71- 75 F5.3 g/cm3 rho Density
77- 81 F5.3 g/cm3 E_rho Error on rho (upper value) (1)
83- 87 F5.3 g/cm3 e_rho Error on rho (lower value) (1)
89- 93 F5.3 [cm/s2] logg Surface gravity
95- 99 F5.3 [cm/s2] E_logg Error on logg (upper value) (1)
101-105 F5.3 [cm/s2] e_logg Error on logg (lower value) (1)
107-111 F5.3 Lsun L Luminosity (2)
113-117 F5.3 Lsun E_L Error on L (upper value) (1)
119-123 F5.3 Lsun e_L Error on L (lower value) (1)
125-129 F5.2 Gyr Age Age
131-134 F4.2 Gyr E_Age Error on Age (upper value) (1)
136-139 F4.2 Gyr e_Age Error on Age (lower value) (1)
141-146 F6.2 pc Dist Distance
148-152 F5.2 pc E_Dist Error on Dist (upper value) (1)
154-158 F5.2 pc e_Dist Error on Dist (lower value) (1)
160-174 A15 --- Notes Literature sources of confirmed or validated
exoplanets
175 A1 --- n_Notes [b] Note (3)
177-260 A84 --- Ref Reference(s)
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Note (1): Additional systematic uncertainties can be accounted for
(see Sections 4.2, 4.3, and 4.4):
from input physics of 0.8% (density), 0.7% (radius), 2.3% (mass), 9.6% (age);
from choice of observables of 0.3% (density and radius), 1% (mass), and
7% (age);
from fitting algorithms and codes of 1% (density and radius), 2% (mass),
and 9% (age);
from the initial helium abundance of 1.7% (density), 1.6% (radius),
3.6% (mass), and 16.8% (age).
Note (2): Solar luminosity used L☉=3.846x1033(erg/s).
Note (3): b: Ephemeris match indicates contamination, see CFOP website
(https://cfop.ipac.caltech.edu/home/).
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Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- KOI KOI number
6- 13 I8 --- KIC KIC number
15- 19 F5.3 Msun Mass Mass
21- 25 F5.3 Msun e_Mass rms uncertainty on Mass
27- 31 F5.3 Rsun Radius Radius
33- 37 F5.3 Rsun e_Radius rms uncertainty on Radius
39- 43 F5.3 g/cm3 rho Density
45- 49 F5.3 g/cm3 e_rho rms uncertainty on rho
51- 55 F5.3 [cm/s2] logg Surface gravity
57- 61 F5.3 [cm/s2] e_logg rms uncertainty on logg
63- 67 F5.3 Lsun L Luminosity
69- 73 F5.3 Lsun e_L rms uncertainty on L
75- 80 F6.3 Gyr Age Age
82- 86 F5.3 Gyr e_Age rms uncertainty on Age
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Byte-by-byte Description of file: tablea2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- KOI KOI number
6- 13 I8 --- KIC KIC number
15- 19 F5.3 Msun Mass Mass
21- 25 F5.3 Msun e_Mass rms uncertainty on Mass
27- 31 F5.3 Rsun Radius Radius
33- 37 F5.3 Rsun e_Radius rms uncertainty on Radius
39- 43 F5.3 g/cm3 rho Density
45- 49 F5.3 g/cm3 e_rho rms uncertainty on rho
51- 55 F5.3 [cm/s2] logg Surface gravity
57- 61 F5.3 [cm/s2] e_logg rms uncertainty on logg
63- 67 F5.3 Lsun L Luminosity
69- 73 F5.3 Lsun e_L rms uncertainty on L
75- 80 F6.3 Gyr Age Age
82- 86 F5.3 Gyr e_Age rms uncertainty on Age
88- 92 F5.3 --- Yini Initial Y abundance
94- 98 F5.3 --- e_Yini rms uncertainty on Yini
100-105 F6.4 --- Zini Initial Z abundance
107-112 F6.4 --- e_Zini rms uncertainty on Zini
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Byte-by-byte Description of file: tablea3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- KOI KOI number
6- 13 I8 --- KIC KIC number
15- 19 F5.3 Msun Mass Mass
21- 25 F5.3 Msun e_Mass rms uncertainty on Mass
27- 31 F5.3 Rsun Radius Radius
33- 37 F5.3 Rsun e_Radius rms uncertainty on Radius
39- 43 F5.3 g/cm3 rho Density
45- 49 F5.3 g/cm3 e_rho rms uncertainty on rho
51- 55 F5.3 [cm/s2] logg Surface gravity
57- 61 F5.3 [cm/s2] e_logg rms uncertainty on logg
63- 67 F5.3 Lsun L Luminosity
69- 73 F5.3 Lsun e_L rms uncertainty on L
75- 80 F6.3 Gyr Age Age
82- 86 F5.3 Gyr e_Age rms uncertainty on Age
88- 92 F5.3 --- Yini Initial Y abundance
94- 98 F5.3 --- e_Yini rms uncertainty on Yini
100-105 F6.4 --- Zini Initial Z abundance
107-112 F6.4 --- e_Zini rms uncertainty on Zini
114-117 F4.2 [-] [alpha/Fe] Abundance [α/Fe]
119-122 F4.2 [-] e_[alpha/Fe] rms uncertainty on [alpha/Fe]
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 15-Feb-2016