  The work reported here demonstrates that it is possible to accurately
determine surface gravities of $\delta$ Sct stars using the frequency content
from high precision photometry and a measurement of the parallax. Using a
sample of 10 eclipsing binary systems with a $\delta$ Sct component and the
unique $\delta$ Sct star discovered with a transiting planet, WASP-33, we were
able to refine the $\Delta\nu-\bar\rho$ relation. Using this relation and
parallaxes, we obtained independent values for the masses and radii, allowing
us to calculate the surface gravities without any constraints from
spectroscopic or binary analysis. A remarkably good agreement was found between
our results and those published, extracted from the analysis of the radial
velocities and light curves of the systems. This reinforces the potential of
$\Delta\nu$ as a valuable observable for $\delta$ Sct stars and settles the
degeneracy problem for the $\log g$ determination through spectroscopy.
