Volume 543, July 2012
|Number of page(s)||55|
|Section||Stellar structure and evolution|
|Published online||27 June 2012|
Oscillation mode frequencies of 61 main-sequence and subgiant stars observed by Kepler⋆
1 Univ Paris-Sud, Institut d’Astrophysique Spatiale, UMR 8617, CNRS, Bâtiment 121, 91405 Orsay Cedex, France
2 Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106-4030, USA
3 School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK
4 Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot, IRFU/SAp, Centre de Saclay, 91191 Gif-sur-Yvette Cedex, France
5 Institute for Computational Astrophysics, Department of Astronomy & Physics, Saint Mary’s University, Halifax, NS B3H 3C3, Canada
6 Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400005, India
7 Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, New South Wales 2006, Australia
8 Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, 8000 Aarhus C, Denmark
9 Centro de Astrofísica and Faculdade de Ciências, Universidade do Porto, rua das Estrelas, 4150-762 Porto, Portugal
10 Department of Astronomy, Yale University, PO Box 208101, New Haven CT 06520-8101, USA
11 Astronomical Institute “Anton Pannekoek”, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands
12 Instituto de Astrofísica de Canarias, 38205 La Laguna, Tenerife, Spain
13 Universidad de La Laguna, Dpto de Astrofísica, 38206 La Laguna, Tenerife, Spain
14 Université de Nice Sophia-Antipolis, CNRS UMR 6202, Observatoire de la Côte d’Azur, BP 4229, 06304 Nice Cedex 4, France
15 Institut de Recherche en Astrophysique et Planétologie, CNRS, 14 avenue E. Belin, 31400 Toulouse, France
16 Université de Toulouse, UPS-OMP, IRAP, 31400 Toulouse, France
17 High Altitude Observatory, NCAR, PO Box 3000, Boulder, CO 80307, USA
18 Max Planck Institute for Astrophysics, Karl-Schwarzschild-Str. 1, 85748 Garching bei München, Germany
19 Center for Exoplanets and Habitable Worlds, The Pennsylvania State University, University Park, PA 16802, USA
20 Orbital Sciences Corporation/NASA Ames Research Center, Moffett Field, CA 94035, USA
21 SETI Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA
22 Bay Area Environmental Research Institute/NASA Ames Research Center, Moffett Field, CA 94035, USA
Received: 2 February 2012
Accepted: 18 April 2012
Context. Solar-like oscillations have been observed by Kepler and CoRoT in several solar-type stars, thereby providing a way to probe the stars using asteroseismology
Aims. We provide the mode frequencies of the oscillations of various stars required to perform a comparison with those obtained from stellar modelling.
Methods. We used a time series of nine months of data for each star. The 61 stars observed were categorised in three groups: simple, F-like, and mixed-mode. The simple group includes stars for which the identification of the mode degree is obvious. The F-like group includes stars for which the identification of the degree is ambiguous. The mixed-mode group includes evolved stars for which the modes do not follow the asymptotic relation of low-degree frequencies. Following this categorisation, the power spectra of the 61 main-sequence and subgiant stars were analysed using both maximum likelihood estimators and Bayesian estimators, providing individual mode characteristics such as frequencies, linewidths, and mode heights. We developed and describe a methodology for extracting a single set of mode frequencies from multiple sets derived by different methods and individual scientists. We report on how one can assess the quality of the fitted parameters using the likelihood ratio test and the posterior probabilities.
Results. We provide the mode frequencies of 61 stars (with their 1-σ error bars), as well as their associated échelle diagrams.
Key words: asteroseismology / stars: solar-type / stars: oscillations
Appendices are available in electronic form at http://www.aanda.org
© ESO, 2012
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