Asteroseismic fundamental properties of solar-type stars observed by the NASA Kepler mission

Research output: Contribution to journalArticlepeer-review

Authors

  • S. Basu
  • D. Huber
  • A. Serenelli
  • L. Casagrande
  • V. Silva Aguirre
  • O. L. Creevey
  • L. Gizon
  • C. Karoff
  • R. Lutz
  • J. P. Marques
  • D. Stello
  • M. D. Suran
  • D. Pricopi
  • T. S. Metcalfe
  • M. J P F G Monteiro
  • J. Molenda-Zakowicz
  • T. Appourchaux
  • J. Christensen-Dalsgaard
  • R. A. García
  • G. Houdek
  • H. Kjeldsen
  • A. Bonanno
  • Tiago Campante
  • E. Corsaro
  • P. Gaulme
  • S. Hekker
  • S. Mathur
  • B. Mosser
  • C. Régulo
  • D. Salabert

Colleges, School and Institutes

External organisations

  • Aarhus Universitet
  • University of Sydney
  • Universidade do Porto
  • Astronomical Institute 'Anton Pannekoek'
  • Université Paris Denis Diderot
  • Institute for Astronomy (IfA), University of Vienna, Türkenschanzstrasse 17, 1180 Vienna, Austria ; Instituut voor Sterrenkunde, K.U. Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
  • INAF-Osservatorio Astrofisico di Catania
  • Uniwersytet Wroclawski
  • Australian National University
  • NASA Ames Research Center, MS 244-30, Moffett Field, CA 94035, USA
  • Facultad de Ciències
  • Campus UAB
  • Max-Planck-Institut für Astrophysik
  • Georg August Universitaet
  • TUBS, Braunschweig, D-38106, and Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, Germany); AH(School of Earth and Space Sciences, University of Science and Technology of China, Hefei, China
  • Université de Nice Sophia-Antipolis
  • Laboratoire Lagrange
  • Institut d'Astrophysique Spatiale (IAS)
  • Institut d'Astrophysique Spatiale, Université Paris XI - CNRS (UMR8617), Batiment 121, 91405 Orsay Cedex, France
  • Sydney Institute for Astronomy (SIfA)
  • Astronomical Institute
  • University of Wrocław
  • CEA DSM CNRS Univ Paris Diderot
  • Instituut voor Sterrenkunde, K.U. Leuven, Belgium
  • Catholic University of Leuven
  • Department of Astronomy
  • University of Amsterdam
  • National Center for Atmospheric Research
  • NCAR
  • LESIA
  • CNRS, CRAN UMR 7039 France
  • Instituto de Astrofísica de Canarias (IAC)
  • Instituto de Astrofísica de Canarias, E-38200 La Laguna, Spain ; Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Spain
  • Yale University
  • NASA Ames Research Center
  • Instituto de Cièncias Del Espacio (CSIC-IEEC)
  • Mount Stromlo Observatory
  • Université Côte d’Azur
  • Astronomical Institute of the Romanian Academy
  • Space Science Institute
  • INAF-Astrophysical Observatory of Catania
  • New Mexico State University Las Cruces
  • MSC 4500
  • Astronomical Institute Anton Pannekoek
  • Universidad de La Laguna
  • UMR7293

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, T eff, were available for the entire ensemble from complementary photometry; spectroscopic estimates of T eff 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 homogenous 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.

Details

Original languageEnglish
Article number1
JournalAstrophysical Journal. Supplement Series
Volume210
Issue number1
Publication statusPublished - 1 Jan 2014

Keywords

  • asteroseismology, methods: data analysis, stars: fundamental parameters, stars: interiors