  We analyze the impact on the Galactic nitrogen abundances of using a new set
of low and intermediate mass star yields. These yields have a significant yield
of primary nitrogen from intermediate mass stars. We use these yields as an
input to a Galactic Chemical Evolution model and study the nitrogen abundances
in the halo and in the disc, and compare them with models obtained using other
yield sets and with a large amount of observational data. We find that, using
these new yields, our model adequately reproduce the observed trends. In
particular, these yields solve the historical problem of the evolution of
nitrogen, giving the right level of relative abundance N/O by the production of
a primary component in intermediate mass stars. Moreover, using different
evolutionary rates in each radial region of the Galaxy, we may explain the
observed N dispersion.
