| In the 1920s, De Vaucouleurs proposed the denisty of matter in the universe obeys a power law relation: denoting by D(r) the density of matter a distance r from the observer, De Vaucouleurs' law is |
| D(r) = k⋅r3-d |
| where d is the dimension of the distribution of matter. |
| A reassuring consequence of this relationship is that there are no preferred observers. |
| "We're nothing special" can be achieved by hierarchical, a well as homogeneous, cosmologies. |
Return to Large-Scale Distribution of Galaxies.