J/MNRAS/480/467 Surface gravities for 15 000 Kepler stars (Pande+, 2018)
Surface gravities for 15 000 Kepler stars measured from stellar granulation and
validated with Gaia DR2 parallaxes.
Pande D., Bedding T.R., Huber D., Kjeldsen H.
<Mon. Not. R. Astron. Soc., 480, 467-472 (2018)>
=2018MNRAS.480..467P 2018MNRAS.480..467P (SIMBAD/NED BibCode)
ADC_Keywords: Asteroseismology ; Stars, fundamental
Keywords: asteroseismology - stars: fundamental parameters - stars: oscillations
Abstract:
We have developed a method to estimate surface gravity (log g) from
light curves by measuring the granulation background, similar to the
'flicker' method by Bastien et al. (2016ApJ...818...43B 2016ApJ...818...43B, Cat.
J/ApJ/818/43) but working in the Fourier power spectrum. We calibrated
the method using Kepler stars for which asteroseismology has been
possible with short-cadence data, demonstrating a precision in log g
of about 0.05dex. We also derived a correction for white noise as a
function of Kepler magnitude by measuring white noise directly from
observations. We then applied the method to the same sample of
long-cadence stars as Bastien et al. We found that about half the
stars are too faint for the granulation background to be reliably
detected above the white noise. We provide a catalogue of log g values
for about 15000 stars having uncertainties better than 0.5dex. We
used Gaia DR2 parallaxes to validate that granulation is a powerful
method to measure log g from light curves. Our method can also be
applied to the large number of light curves collected by K2 and TESS.
Description:
We have estimated logg from Kepler light curves by measuring the
granulation background, similar to the 'flicker' method by Bastien et
al. (2016ApJ...818...43B 2016ApJ...818...43B, Cat. J/ApJ/818/43) but working in the
Fourier power spectrum. We established a calibration for white noise
as a function of magnitude and calibrated the granulation power using
the asteroseismic short-cadence sample. Applying the method to the
sample of 28000 long-cadence stars studied by Bastien et al.
(2016ApJ...818...43B 2016ApJ...818...43B, Cat. J/ApJ/818/43), we found about half the
stars to be too faint for the granulation background to be reliably
detected above the white noise. We have provided an electronic
catalogue of logg values (with uncertainties) for about 15000 stars
having logg uncertainties better than 0.5dex.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 104 15109 Estimates of granulation power, vmax and logg
for 15109 stars using Kepler long-cadence data
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/ApJ/818/43 : Stellar surface gravity measures of KIC stars (Bastien+, 2016)
J/ApJS/229/30 : Revised stellar properties of Q1-17 Kepler targets
(Mathur+, 2017)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 8 I8 --- KIC Kepler Input Catalog identifier (Cat. V/133)
10- 18 F9.6 mag Kpmag Kepler magnitude
20- 23 I4 K Teff Effective temperature (1)
25- 27 I3 K e_Teff Effective temperature error (1)
29- 41 F13.6 ppm2/uHz Pgran Granulation power
43- 58 F16.6 ppm2/uHz e_Pgran Granulation power error
60- 70 F11.6 uHz vmax Frequency of maximum oscillation power
72- 84 F13.6 uHz e_vmax Frequency of maximum oscillation power error
86- 93 F8.6 [cm/s2] logg Surface gravity
95-104 F10.6 [cm/s2] e_logg Surface gravity error
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Note (1): Effective temperatures are taken from Mathur et al.
(2017ApJS..229...30M 2017ApJS..229...30M, Cat. J/ApJS/229/30)
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 09-May-2022