  We determine the spatial distribution function of galaxies from a wide range
of samples in the 2MASS survey. The results agree very well with the form of
the distribution predicted by the theory of cosmological gravitational
many-body galaxy clustering. On large scales we find a value of the clustering
parameter b = 0.867 +/- 0.026, in agreement with b = 0.83 +/- 0.05 found
previously for the Pisces-Perseus supercluster. We measure b(theta) as a
function of scale, since this is a powerful test of the applicability of
computer simulations. The results suggest that when galaxies clustered they
were usually surrounded by individual, rather than by communal haloes.
