  Using population synthesis tools we create a synthetic Kepler Input Catalogue
(KIC) and subject it to the Kepler Stellar Classification Program (SCP) method
for determining stellar parameters such as the effective temperature Teff and
surface gravity g. We achieve a satisfactory match between the synthetic KIC
and the real KIC in the log g vs log Teff diagram, while there is a significant
difference between the actual physical stellar parameters and those derived by
the SCP of the stars in the synthetic sample. We find a median difference
\Delta Teff=+500K and \Delta log g =-0.2dex for main-sequence stars, and \Delta
Teff=+50K and \Delta log g =-0.5dex for giants, although there is a large
variation across parameter space. For a MS star the median difference in g
would equate to a ~3% increase in stellar radius and a consequent ~3%
overestimate of the radius for any transiting exoplanet. We find no significant
difference between \Delta Teff and \Delta log g for single stars and the
primary star in a binary system. We also re-created the Kepler target selection
method and found that the binary fraction is unchanged by the target selection.
Binaries are selected in similar proportions to single star systems; the
fraction of MS dwarfs in the sample increases from about 75% to 80%, and the
giant star fraction decreases from 25% to 20%.
