期刊
ASTROPHYSICAL JOURNAL
卷 885, 期 2, 页码 -出版社
IOP Publishing Ltd
DOI: 10.3847/1538-4357/ab44a9
关键词
asteroseismology; catalogs; parallaxes; stars: fundamental parameters; stars: low-mass
资金
- NASA [80NSSC18K0391, NNX17AJ40G]
- National Science Foundation [AST-1717000, NSF PHY-1748958]
- Australian Research Council Future Fellowship [FT1400147]
- Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) [CE170100013]
- MICINN [ESP2017-82674-R]
- Generalitat de Catalunya [2017-SGR-1131]
- Heising-Simons Foundation
- Alfred P. Sloan Foundation
- U.S. Department of Energy Office of Science
- Center for High-Performance Computing at the University of Utah
- 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
- Korean Participation Group
- 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 compare radii based on Gaia parallaxes to radii based on asteroseismic scaling relations for ?300 dwarfs and subgiants and ?3600 first-ascent giants from the Kepler mission. Systematics due to temperature, bolometric correction, extinction, asteroseismic radius, and the spatially correlated Gaia parallax zero-point contribute to a 2% systematic uncertainty on the agreement in Gaia?asteroseismic radius. We find that dwarf and giant scaling radii are on a parallactic scale at the level of ;2.0% (syst.) (giants), supporting the accuracy and precision of scaling relations. In total, the 2% agreement that we find holds for stars spanning radii between 0.8
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