Asteroseismic constraints for Gaia
  Distances from the Gaia mission will no doubt improve our understanding of
stellar physics by providing an excellent constraint on the luminosity of the
star. However, it is also clear that high precision stellar properties from,
for example, asteroseismology, will also provide a needed input constraint in
order to calibrate the methods that Gaia will use, e.g. stellar models or
GSP_phot. For solar-like stars (F, G, K IV/V), asteroseismic data delivers at
the least two very important quantities: (1) the average large frequency
separation <Delta_nu> and (2) the frequency corresponding to the maximum of the
modulated-amplitude spectrum nu_max. Both of these quantities are related
directly to stellar parameters (radius and mass) and in particular their
combination (gravity and density). We show how the precision in <Delta_nu>,
nu_max, and atmospheric parameters T_eff and [Fe/H] affect the determination of
gravity (log g) for a sample of well-known stars. We find that log g can be
determined within less than 0.02 dex accuracy for our sample while considering
precisions in the data expected for V<12 stars from Kepler data. We also derive
masses and radii which are accurate to within 1sigma of the accepted values.
This study validates the subsequent use of all of the available asteroseismic
data on main sequence solar-like stars from the Kepler field (>500 IV/V stars)
in order to provide a very important constraint for Gaia calibration of
GSP_phot through the use of log g. We note that while we concentrate on IV/V
stars, both the CoRoT and Kepler fields contain asteroseismic data on thousands
of giant stars which will also provide useful calibration measures.
