期刊
ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
卷 239, 期 2, 页码 -出版社
IOP Publishing Ltd
DOI: 10.3847/1538-4365/aaebfd
关键词
stars abundances; stars: fundamental parameters; stars: oscillations (including pulsations)
资金
- National Science Foundation [NSF PHY17-48958]
- NASA [NNX17AJ40G, NNX15AF13G, NNX14AB92G]
- National Research Foundation of Korea [2017R1A5A1070354]
- European Union's Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant [664931]
- UK Science and Technology Facilities Council (STFC)
- NASA through the Astrophysics Division of the Science Mission Directorate [16-XRP16 2-0004]
- CNES
- CNESDAGH
- Spanish Ministry of Economy and Competitiveness (MINECO) [AYA-2014-58082-P, AYA-2017-88254-P]
- PRIN INAF [2014CRA1.05.01.94.05]
- Crafoord Foundation
- Stiftelsen Olle Engkvist Byggmastare
- European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC [338251]
- NSF [AST-1411685]
- Ramon y Cajal fellowship [RYC-2015-17697]
- Premium Postdoctoral Research Program of the Hungarian Academy of Sciences
- Hungarian NKFI grants of the Hungarian National Research, Development and Innovation Office [K-119517]
- Australian Research Council Future Fellowship [FT1400147]
- U.S. National Science Foundation [PHY-1430152]
- Alfred P. Sloan Foundation
- U.S. Department of Energy Office of Science
- Brazilian Participation Group
- Carnegie Institution for Science
- Carnegie Mellon University
- Chilean Participation Group
- French Participation Group
- Harvard-Smithsonian Center for Astrophysics
- Instituto de Astrofisica de Canarias
- Johns Hopkins University
- Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo
- Lawrence Berkeley National Laboratory
- Leibniz Institut fur Astrophysik Potsdam (AIP)
- Max-Planck-Institut fur Astronomie (MPIA Heidelberg)
- Max-Planck-Institut fur Astrophysik (MPA Garching)
- Max-Planck-Institut fur Extraterrestrische Physik (MPE)
- National Astronomical Observatories of China
- New Mexico State University
- New York University
- University of Notre Dame
- Observatario Nacional/MCTI
- Ohio State University
- Pennsylvania State University
- Shanghai Astronomical Observatory
- United Kingdom Participation Group
- Universidad Nacional Autonoma de Mexico
- University of Arizona
- University of Colorado Boulder
- University of Oxford
- University of Portsmouth
- University of Utah
- University of Virginia
- University of Washington
- University of Wisconsin
- Vanderbilt University
- Yale University
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 (Av) scaling relation, and we calibrate the zero-point of the frequency of the maximum power (vmax) 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.
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