Asteroseismology and Gaia: Testing Scaling Relations Using 2200 Kepler Stars with TGAS Parallaxes

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 binari...

Full description

Saved in:

Bibliographic Details
Published in:	The Astrophysical journal 2017-08, Vol.844 (2), p.102
Main Authors:	Huber, Daniel, Zinn, Joel, Bojsen-Hansen, Mathias, Pinsonneault, Marc, Sahlholdt, Christian, Serenelli, Aldo, Aguirre, Victor Silva, Stassun, Keivan, Stello, Dennis, Tayar, Jamie, Bastien, Fabienne, Bedding, Timothy R., Buchhave, Lars A., Chaplin, William J., Davies, Guy R., García, Rafael A., Latham, David W., Mathur, Savita, Mosser, Benoit, Sharma, Sanjib
Format:	Article
Language:	eng
Subjects:	Astrophysics ASTROPHYSICS, COSMOLOGY AND ASTRONOMY COMPARATIVE EVALUATIONS CORRECTIONS DISTANCE ECLIPSE FUNCTIONS LUMINOSITY METALLICITY Offsets OSCILLATIONS Parallax parallaxes Physics POPULATIONS STARS stars: distances stars: fundamental parameters stars: late-type stars: oscillations Stellar populations Stellar seismology Systematic errors techniques: photometric
Online Access:	Get full text
Tags:	Add Tag No Tags, Be the first to tag this record!

Description
Summary:	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 mas ( 90%-98% of the TGAS sample). The observed differences in our sample can furthermore be partially compensated by adopting a hotter 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 . We find no significant offset for main-sequence ( ) and low-luminosity RGB stars ( 3-8 ), but seismic radii appear to be systematically underestimated by 5% for subgiants ( 1.5-3 ). We find no systematic errors as a function of metallicity between to dex, and show tentative evidence that corrections to the scaling relation for the large frequency separation ( ) improve the agreement with TGAS for RGB stars. Finally, we demonstrate that beyond 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.
ISSN:	0004-637X 1538-4357