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Early attempts to apply asteroseismology to study the Galaxy have alreadyshown unexpected discrepancies for the mass distribution of stars between theGalactic models and the data; a result that is still unexplained. Here, werevisit the analysis of the asteroseismic sample of dwarf and subgiant starsobserved by Kepler and investigate in detail the possible causes for thereported discrepancy. We investigate two models of the Milky Way based onstellar population synthesis, Galaxia and TRILEGAL. In agreement with previousresults, we find that TRILEGAL predicts more massive stars compared to Galaxia,and that TRILEGAL predicts too many blue stars compared to 2MASS observations.Both models fail to match the distribution of the stellar sample in $(\logg,T_{\rm eff})$ space, pointing to inaccuracies in the models and/or theassumed selection function. When corrected for this mismatch in $(\log g,T_{\rmeff})$ space, the mass distribution calculated by Galaxia is broader and themean is shifted toward lower masses compared to that of the observed stars.This behaviour is similar to what has been reported for the Kepler red giantsample. The shift between the mass distributions is equivalent to a change of2\% in $\nu_{\rm max}$, which is within the current uncertainty in the$\nu_{\rm max}$ scaling relation. Applying corrections to the $\Delta \nu$scaling relation predicted by the stellar models makes the observed massdistribution significantly narrower, but there is no change to the mean.

Stellar population synthesis based modelling of the Milky Way using asteroseismology of dwarfs and subgiants from Kepler