  We study the effect of different Type Ia SN nucleosynthesis prescriptions on
the Milky Way chemical evolution. To this aim, we run detailed one-infall and
two-infall chemical evolution models, adopting a large compilation of yield
sets corresponding to different white dwarf progenitors (near-Chandrasekar and
sub-Chandrasekar) taken from the literature. We adopt a fixed delay time
distribution function for Type Ia SNe , in order to avoid degeneracies in the
analysis of the different nucleosynthesis channels. We also combine yields for
different Type Ia SN progenitors in order to test the contribution to chemical
evolution of different Type Ia SN channels. The results of the models are
compared with recent LTE and NLTE observational data. We find that "classical"
W7 and WDD2 models produce Fe masses and [$\alpha$/Fe] abundance patterns
similar to more recent and physical near-Chandrasekar and sub- Chandrasekar
models. For Fe-peak elements, we find that the results strongly depend either
on the white dwarf explosion mechanism (deflagration-to-detonation, pure
deflagration, double detonation) or on the initial white dwarf conditions
(central density, explosion pattern). The comparison of chemical evolution
model results with observations suggests that a combination of
near-Chandrasekar and sub-Chandrasekar yields is necessary to reproduce the
data of V, Cr, Mn and Ni, with different fractions depending on the adopted
massive stars stellar yields. This comparison also suggests that NLTE and
singly ionised abundances should be definitely preferred when dealing with most
of Fe-peak elements at low metallicity.
