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We confirm that the number of globular clusters (GCs), N$_{GC}$, is anexcellent tracer of their host galaxy's halo virial mass M$_{vir}$. The simplelinear relation M$_{vir} = 5 \times 10^9$ M$_{\odot} \times$ N$_{GC}$ fits thedata perfectly from M$_{vir} = 10^{10}$ M$_{\odot}$ to M$_{vir} = 2 \times10^{15}$ M$_{\odot}$. This result is independent of galaxy morphology andextends statistically into the dwarf galaxy regime with M$_{vir} = 10^8 -10^{10}$ M$_{\odot}$, including the extreme ultra diffuse galaxy DF44. As thiscorrelation does not depend on GC mass it is ideally suited for high-precisiondeterminations of M$_{vir}$. The linearity is most simply explained bycosmological merging of a high-redshift halo seed population that hosted onaverage one GC per $5 \times 10^8$ M$_{\odot}$ of dark matter. We show thathierarchical merging is also extremely powerful in restoring a linearcorrelation and erasing signatures of even a strong secular evolution of GCsystems. The cosmological merging scenario also implies a strong decline of thescatter in $N_{GC}$ with increasing virial mass $\delta N_{GC}/N_{GC} \simM_{vir}^{-1/2}$ in contrast with the observations that show a roughly constantscatter, independent of virial mass. This discrepancy can be explained iferrors in determining virial masses from kinematical tracers and gravitationallensing are on the order of a factor of 2. GCs in dwarf satellite galaxies posea serious problem for high-redshift GC formation scenarios; the dark halomasses of dwarf galaxies hosting GCs therefore might need to be an order ofmagnitude larger than currently estimated.

High-Precision Dark Halo Virial Masses from Globular Cluster Numbers: Implications for Globular Cluster Formation and Galaxy Assembly