TY - JOUR
T1 - Asteroseismology and Gaia
T2 - Testing scaling relations using 2200 Kepler stars with TGAS parallaxes
AU - Huber, Daniel
AU - Zinn, Joel
AU - Bojsen-Hansen, Mathias
AU - Pinsonneault, Marc
AU - Sahlholdt, Christian
AU - Serenelli, Aldo
AU - Aguirre, Victor Silva
AU - Stassun, Keivan
AU - Stello, Dennis
AU - Tayar, Jamie
AU - Bastien, Fabienne
AU - Bedding, Timothy R.
AU - Buchhave, Lars A.
AU - Chaplin, William J.
AU - Davies, Guy R.
AU - García, Rafael A.
AU - Latham, David W.
AU - Mathur, Savita
AU - Mosser, Benoit
AU - Sharma, Sanjib
N1 - Funding Information:
We thank Willie Torres, Yvonne Elsworth, and our anonymous referee for helpful comments and discussions, as well as the entire Kepler and Gaia teams for making this paper possible. D.H. acknowledges support by the Australian Research Council’s Discovery Projects funding scheme (project number DE140101364) and support by the National Aeronautics and Space Administration under Grant NNX14AB92G issued through the Kepler Participating Scientist Program. A.S. is partially supported by grant ESP2015-66134-R (MINECO). V.S.A. acknowledges support from VILLUM FONDEN (research grant 10118). W.J.C. and G.R.D. acknowledge support from the UK Science and Technology Facilities Council. R.A.G. acknowledges the support of CNES. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant agreement no.: DNRF106). S.M. acknowledges support from NASA grants NNX12AE17G, NNX15AF13G, and NNX14AB92G, as well as NSF grant AST-1411685.
Funding Information:
This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/ gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/ dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular, the institutions participating in the Gaia Multilateral Agreement. Funding for the Kepler Mission is provided by NASA’s Science Mission Directorate. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. 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 acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS web site is http:// www.sdss.org. SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrofísica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astro-nomie (MPIA Heidelberg), Max-Planck-Institut für Astrophy-sik (MPA Garching), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatories of China, New Mexico State University, New York University, University of Notre Dame, Observatório Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma de México, 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, and Yale University.
Publisher Copyright:
© 2017 The American Astronomical Society. All rights reserved.
PY - 2017
Y1 - 2017
N2 - We present a comparison of parallaxes and radii from asteroseismology and Gaia DR1 (TGAS) for 2200 Kepler stars spanning from the main sequence to the red-giant branch. We show that previously identified offsets between TGAS parallaxes and distances derived from asteroseismology and eclipsing binaries have likely been overestimated for parallaxes ≲5-10 mas (≈90%-98% of the TGAS sample). The observed differences in our sample can furthermore be partially compensated by adopting a hotter Teff scale (such as the infrared flux method) instead of spectroscopic temperatures for dwarfs and subgiants. Residual systematic differences are at the ≈2% level in parallax across three orders of magnitude. We use TGAS parallaxes to empirically demonstrate that asteroseismic radii are accurate to ≈5% or better for stars between ≈0.8-8 R⊙. We find no significant offset for main-sequence (≲1.5 R⊙) and low-luminosity RGB stars (≈3-8 R⊙), but seismic radii appear to be systematically underestimated by ≈5% for subgiants (≲1.5-3 R⊙). We find no systematic errors as a function of metallicity between [Fe H] ≈ -0.8 to +0.4 dex, and show tentative evidence that corrections to the scaling relation for the large frequency separation (Δν) improve the agreement with TGAS for RGB stars. Finally, we demonstrate that beyond ≈3 kpc asteroseismology will provide more precise distances than end-of-mission Gaia data, highlighting the synergy and complementary nature of Gaia and asteroseismology for studying galactic stellar populations.
AB - We present a comparison of parallaxes and radii from asteroseismology and Gaia DR1 (TGAS) for 2200 Kepler stars spanning from the main sequence to the red-giant branch. We show that previously identified offsets between TGAS parallaxes and distances derived from asteroseismology and eclipsing binaries have likely been overestimated for parallaxes ≲5-10 mas (≈90%-98% of the TGAS sample). The observed differences in our sample can furthermore be partially compensated by adopting a hotter Teff scale (such as the infrared flux method) instead of spectroscopic temperatures for dwarfs and subgiants. Residual systematic differences are at the ≈2% level in parallax across three orders of magnitude. We use TGAS parallaxes to empirically demonstrate that asteroseismic radii are accurate to ≈5% or better for stars between ≈0.8-8 R⊙. We find no significant offset for main-sequence (≲1.5 R⊙) and low-luminosity RGB stars (≈3-8 R⊙), but seismic radii appear to be systematically underestimated by ≈5% for subgiants (≲1.5-3 R⊙). We find no systematic errors as a function of metallicity between [Fe H] ≈ -0.8 to +0.4 dex, and show tentative evidence that corrections to the scaling relation for the large frequency separation (Δν) improve the agreement with TGAS for RGB stars. Finally, we demonstrate that beyond ≈3 kpc asteroseismology will provide more precise distances than end-of-mission Gaia data, highlighting the synergy and complementary nature of Gaia and asteroseismology for studying galactic stellar populations.
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U2 - 10.3847/1538-4357/aa75ca
DO - 10.3847/1538-4357/aa75ca
M3 - Article
AN - SCOPUS:85027411977
VL - 844
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2
M1 - 102
ER -