We present a catalog of stellar properties for a large sample of 6676 evolved stars with Apache Point Observatory Galactic Evolution Experiment spectroscopic parameters and Kepler asteroseismic data analyzed using five independent techniques. Our data include evolutionary state, surface gravity, mean density, mass, radius, age, and the spectroscopic and asteroseismic measurements used to derive them. We employ a new empirical approach for combining asteroseismic measurements from different methods, calibrating the inferred stellar parameters, and estimating uncertainties. With high statistical significance, we find that asteroseismic parameters inferred from the different pipelines have systematic offsets that are not removed by accounting for differences in their solar reference values. We include theoretically motivated corrections to the large frequency spacing (Δν) scaling relation, and we calibrate the zero-point of the frequency of the maximum power (ν max) relation to be consistent with masses and radii for members of star clusters. For most targets, the parameters returned by different pipelines are in much better agreement than would be expected from the pipeline-predicted random errors, but 22% of them had at least one method not return a result and a much larger measurement dispersion. This supports the usage of multiple analysis techniques for asteroseismic stellar population studies. The measured dispersion in mass estimates for fundamental calibrators is consistent with our error model, which yields median random and systematic mass uncertainties for RGB stars of order 4%. Median random and systematic mass uncertainties are at the 9% and 8% level, respectively, for red clump stars.
Bibliographical noteFunding Information:
Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website ishttp://www.sdss.org.
We would like to acknowledge an anonymous referee whose insightful comments helped to improve the paper. M.H.P. was a visitor at KITP while working on the manuscript and acknowledges support from the National Science Foundation under grant No. NSF PHY17-48958. M.H.P., J.A.J., J.T., and J.Z. acknowledge support from NASA grants NNX17AJ40G and NNX15AF13G. D.A. acknowledges support provided by the National Research Foundation of Korea (No. 2017R1A5A1070354). E.C. is funded by the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 664931. Y.E. acknowledges the support of the UK Science and Technology Facilities Council (STFC). K.C. and V.S. acknowledge that their work here is supported in part by NASA under grant 16-XRP16 2-0004, issued through the Astrophysics Division of the Science Mission Directorate. R.A.G acknowledges support from CNES. A.G.H. acknowledges support from CNESDAGH, and O.Z. acknowledges support provided by the Spanish Ministry of Economy and Competitiveness (MINECO) under grants AYA-2014-58082-P and AYA-2017-88254-P. L.G. and T.R. acknowledge support from PRIN INAF 2014CRA1.05.01.94.05. D.H. acknowledges support by NASA under grant NNX14AB92G issued through the Kepler Participating Scientist Program. H.J. acknowledges support from the Crafoord Foundation and Stiftelsen Olle Engkvist Byggmästare. S.K. acknowledges support from the European Research Council under the European Community’s Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 338251 (StellarAges). S.M. acknowledges support from NASA grant NNX15AF13G and NSF grant AST-1411685 and the Ramon y Cajal fellowship number RYC-2015-17697. S.z.M. has been supported by the Premium Postdoctoral Research Program of the Hungarian Academy of Sciences, and by the Hungarian NKFI grants K-119517 of the Hungarian National Research, Development and Innovation Office. D.S. is the recipient of an Australian Research Council Future Fellowship (project number FT1400147). T.C.B. acknowledges partial support from grant No. PHY-1430152 (Physics Frontier Center/JINA Center for the Evolution of the Elements), awarded by the U.S. National Science Foundation.
© 2018. The American Astronomical Society. All rights reserved.
- stars: abundances
- stars: fundamental parameters
- stars: oscillations (including pulsations)