We analyze the galaxy distribution functions for voids and counts-in-c
ells using the IRAS catalog. Angular diameter scales, the largest prob
ed to date, range from 0.5-degrees to 30-degrees, corresponding to lin
ear diameters less than or similar to 40 h-1 Mpc. The analysis develop
s a new technique which has no free parameters. On all scales, the res
ults agree closely with predictions of simple gravitational galaxy clu
stering. The value of b(pattern) for the IRAS galaxies at a cell diame
ter of 30-degrees is 0.62 +/- 0.03. It is nearly independent of scale
for angular diameters greater than or similar to 20-degrees. We also d
evelop a new method for using the projected distribution functions to
estimate the average amplitude, -epsilon, and scale, r(neg), where the
spatial two-point galaxy correlation function, xi2, becomes negative.
This technique is sensitive to the negative range of xi2 and is indep
endent of the peculiar velocity effects which make measurements of the
spatial correlation function uncertain on some scales. It shows that
a large class of CDM-related models, with linear biasing, appears to b
e inconsistent with the IRAS distribution. We discuss some implication
s for the selection of the IRAS galaxies, the scale invariance of high
er order moments of the IRAS distribution function, and the evidence t
hat initial conditions for galaxy clustering were Gaussian.