  Standard models for deep galaxy counts are based on luminosity functions (LF)
with relatively flat faint end ($\alpha\sim-1.0$). Galaxy counts in the B--band
exceed the prediction of such models by a factor of 2 to more than 5, forcing
the introduction of strong luminosity and/or density evolution. Recently Marzke
et al. (1994a) using the CfA redshift survey sample find that the number of
galaxies in the range $-16<M_{Zw}<-13$ exceeds the extrapolation of a flat
faint end LF by a factor of 2. Here we show that this steep LF substantially
contributes to justify the observed blue galaxy counts without invoking strong
luminosity and/or density evolution. Furthermore we show that taking into
account the variation of the $B-K$ color as a function of the morphological
types and assuming a mean value $<B-K><2.5$ for dwarf galaxies, we reproduce
well also the observed $K$--band deep galaxy counts. This assumption is
supported by the strong correlation we found between $B-K$ color of galaxies
and their infrared absolute magnitude: galaxies become bluer with decreasing
luminosity.
