  We present theoretical mass estimates of $^{26}$Al and $^{60}$Fe throughout
the Galaxy, performed with a numerical chemical evolution model including
detailed nucleosynthesis prescriptions for stable and radioactive nuclides. We
compared the results for several sets of stellar yields taken from the
literature, for massive, low and intermediate mass stars, nova systems (only
for $^{26}$Al) and supernovae Type Ia.We then computed the total masses of
$^{26}$Al and $^{60}$Fe in the Galaxy. We studied the bulge and the disc of the
Galaxy in a galactocentric radius range 0-22 kpc. We assumed that the bulge
region (within 2 kpc) evolved quickly suffering a strong star formation burst,
while the disc formed more slowly and inside-out. We compared our results with
the $^{26}$Al mass observed by the $\gamma$-ray surveys COMPTEL and INTEGRAL to
select the best model. Concerning $^{60}$Fe, we do not have any observed mass
value so we just performed a theoretical prediction for future observations. In
conclusion, low, intermediate mass stars and Type Ia supernovae contribute
negligibly to the two isotopes, while massive stars are the dominant source.
The nova contribution is, however, necessary to reproduce the observations of
$^{26}$Al. Our best model predicts $2.12$ M$_{\odot}$ of $^{26}$Al, in
agreement with observations, while for $^{60}$Fe our best mass estimate is
$\sim 1.05$ M$_{\odot}$. We also predicted the present injection rate of
$^{26}$Al and $^{60}$Fe in the Galaxy and compared it with previous results,
and we found a larger present time injection rate along the disc.
