Given that the distance scale of the GRBs is unknown, the typical representation of the GRB intensity is given in "peak intensity", in photons cm-2 s-1 in a given energy range. If one plots the number of events with peak intensity greater than the abscissa value (i.e. the cumulative function) in a log-log scale, in case of homogeneous distribution of GRBs throughout an Euclidean space (that is, a constant number density and luminosity distribution over the space), one would expect a power law distribution with index -3/2, that interrupts at the sensitivity limit of the instrument. This can be easily understood just thinking that the volume increases as the third power of the distance, while the electromagnetic flux decreases as the square power of the distance. What we observe in a typical representation of the available data, like the one shown in figure 5.2, is that the distribution bends for low peak intensities from the -3/2 trend, due to a paucity of the weaker events. This is an indication that we may be observing the end of the homogeneous spatial distribution. Of course any conclusion must deal with the intrinsic emission mechanism of the GRB emitters, that is still unknown, and with its possible evolution in the cosmological time. What we can exclude on the basis of this measurement is an homogeneous distribution in our Galaxy, with a fixed intrinsic luminosity.