7–dimensional square box is placed on the target galaxy. The center of this box is defined by the observed photometric colors ([*i.e.*]{}, $u-g$, $g-r$, $r-i$, $i-z$), the Right Ascension, Declination and redshift of the target galaxy. The width of the box is dependent on the redshift and photometric errors on the colors of the target galaxy. Once the box is defined, the number of neighboring galaxies is counted within the SDSS main galaxy sample (Strauss et al. 2002) inside this box and this count is reported (see Figure \[colorcolor\]).

2.  The same 7–D box is placed on 100 randomly chosen galaxies, also taken from the SDSS main galaxy spectroscopic sample, that possess similar seeing and reddening values (see Figure \[colorcolor\]). For each of these 100 randomly chosen galaxies, the number of neighboring galaxies is counted (from the SDSS main galaxy sample) inside the box and a distribution of galaxy counts is constructed from these 100 randomly chosen galaxies.

3.  Using this observed distribution of galaxy counts, the probability of obtaining the observed galaxy count around the original target galaxy is computed.

4.  This exercise is repeated for all galaxies in the sample and then rank all these probabilities.

5.  Using 