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 both stable and radioactive nuclides. We compared the results for several sets of stellar yields taken from the literature, either for massive, low and intermediate mass stars, nova systems (only for 26 Al) and supernovae Type Ia, and then computed the total masses of 26 Al and 60 Fe in the Galaxy. In particular, we have studied the bulge and the disc of the Galaxy in a galactocentric radius range between 0 and 22 kpc. We have assumed that the bulge region (between 0 and 2 kpc) evolved very quickly suffering a strong burst of star formation, while the disc formed more slowly and inside-out, in agreement with previous works, which reproduced the majority of observational constraints. We have compared our results with the 26 Al mass observed by the γ-ray surveys COMPTEL and INTEGRAL, in order to select the best model. Concerning 60 Fe, for which we do not have any observed mass value, we have just predicted its mass to provide a theoretical predictions to be confirmed or disproved by future observations. We have found that low and intermediate mass stars as well as Type Ia supernovae contribute negligibly to the two isotopes, while massive stars are the dominant source. The contribution from novae is, however, necessary to reproduce the observed mass of 26 Al, and this is a new result. Our best model predicts a mass of 2.12 M of 26 Al, in agreement with observations, while for 60 Fe our best mass estimate is around ∼ 1.05 M . We have also predicted the present rate of injection of 26 Al and 60 Fe in the Galaxy and compared it with previous results, and we have predicted a larger present time rate of injection along the disc, relative to previous works.