Testing the radius scaling relation with $Gaia$ DR2 in the $Kepler$ field

Abstract

We compare radii based on $Gaia$ parallaxes to asteroseismic scaling relation-based radii of $\sim 300$ dwarfs $\&$ subgiants and $\sim 3600$ 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 $Gaia$-asteroseismic radius agreement. We find that dwarf and giant scaling radii are on a parallactic scale at the $-2.1\%\pm 0.5\%(rand.)\pm 2.0\%(syst.)$ level (dwarfs) and $+1.7\%\pm 0.3\%(rand.)\pm 2.0\%(syst.)$ level (giants), supporting the accuracy and precision of scaling relations in this domain. In total, the $2\%$ agreement that we find holds for stars spanning radii between $0.8R_{\odot }$ and $30R_{\odot }$. We do, however, see evidence for $\text{relative}$ errors in scaling radii between dwarfs and giants at the $4\%\pm 0.6\%$ level, and find evidence of departures from simple scaling relations for radii above $30R_{\odot }$. Asteroseismic masses for very metal-poor stars are still overestimated relative to astrophysical priors, but at a reduced level. We see no trend with metallicity in radius agreement for stars with $-0.5<$ [Fe/H] $<+0.5$. We quantify the spatially-correlated parallax errors in the $Kepler$ field, which globally agree with the $Gaia$ team's published covariance model. We provide $Gaia$ radii, corrected for extinction and the $Gaia$ parallax zero-point for our full sample of $\sim 3900$ stars, including dwarfs, subgiants, and first-ascent giants.

arXiv commentPublished in ApJ

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