[en] Globular clusters (GC) are important objects for tracing the early evolution of a galaxy. We study the relation between the properties of globular cluster systems—as quantified by the GC specific frequency ($S_N$)—and the properties of their host galaxies. In order to understand the origin of the relation between the GC specific frequency ($S_N$) and galaxy mass, we devise a theoretical model for the specific frequency ($S_{N,th}$). GC erosion is considered to be an important aspect for shaping this relation, since observations show that galaxies with low densities have a higher $S_N$, while high density galaxies have a small $S_N$. We construct a model based on the hypothesis that star-formation is clustered and depends on the minimum embedded star cluster mass (${\mathrm{M}}_{\mathrm{e}\mathrm{c}\mathrm{l},\mathrm{m}\mathrm{i}\mathrm{n}}$), the slope of the power-law embedded cluster mass function ($\mathrm{\beta <!--\; ??\; -->}$) and the relation between the star formation rate (SFR) and the maximum star cluster mass (${\mathrm{M}}_{\mathrm{e}\mathrm{c}\mathrm{l},\mathrm{m}\mathrm{a}\mathrm{x}}$). We find an agreement between the primordial value of the specific frequency ($S_{Ni}$) and our model for $\mathrm{\beta <!--\; ??\; -->}$ between 1.5 and 2.5 with ${\mathrm{M}}_{\mathrm{e}\mathrm{c}\mathrm{l},\mathrm{m}\mathrm{i}\mathrm{n}}\le <!--\; ???\; -->{10}^4{\mathrm{M}}_{\odot <!--\; ???\; -->}$.