  Asteroseismology has been extremely successful in determining the properties
of stars in different evolutionary stages with a remarkable level of precision.
However, to fully exploit its potential, robust methods for estimating stellar
parameters are required and independent verification of the results is needed.
In this talk, I present a new technique developed to obtain stellar properties
by coupling asteroseismic analysis with the InfraRed Flux Method. Using two
global seismic observables and multi-band photometry, the technique determines
masses, radii, effective temperatures, bolometric fluxes, and thus distances
for field stars in a self-consistent manner. Applying our method to a sample of
solar-like oscillators in the {\it Kepler} field that have accurate {\it
Hipparcos} parallaxes, we find agreement in our distance determinations to
better than 5%. Comparison with measurements of spectroscopic effective
temperatures and interferometric radii also validate our results, and show that
our technique can be applied to stars evolved beyond the main-sequence phase.
