  We present the \nuk{Al}{26} and \nuk{Fe}{60} yields produced by a generation
of solar metallicity stars ranging in mass between 11 and 120\msun. We discuss
the production sites of these $\gamma$ ray emitters and quantify the relative
contributions of the various components. More specifically we provide the
separate contribution of the wind, the C convective shell and the explosive
Ne/C burning to the total \nuk{Al}{26} yield per each stellar model in our
grid. We provide the contributions of the He convective shell, the C convective
shell and the explosive Ne/C burning to the \nuk{Fe}{60} yield as well. From
these computations we conclude that, at variance with current beliefs,
\nuk{Al}{26} is mainly produced by the explosive C/Ne burning over most of the
mass interval presently analyzed while \nuk{Fe}{60} is mainly produced by the C
convective shell and the He convective shell.
