The angular correlation function is a function which measures the projected clustering of galaxies, due to discrepancies between their actual and expected distributions. The function may be computed as follows: w ( θ ) = 1 N d P d Ω − 1 {\displaystyle w(\theta )={\frac {1}{N}}{\frac {dP}{d\Omega }}-1} , where P {\displaystyle P} represents the conditional probability of finding a galaxy, Ω {\displaystyle \Omega } denotes the solid angle, and N {\displaystyle N} is the mean number density. In a homogeneous universe, the angular correlation scales with a characteristic depth.