We study the relationships between galaxy total luminosity ( M _ { g ^ { \prime } } ) , morphology , color and environment as a function of redshift .
We use a magnitude-limited sample of 65,624 galaxies in the redshift range 0 < z < 1.3 taken from one of the 1 \mbox { $ { } ^ { \circ } $ } \times 1 \mbox { $ { } ^ { \circ } $ } Canada–France–Hawaii Telescope Legacy Survey Deep Fields .
We parametrize galaxy morphology according to the Sérsic index n , taking n > 2 to be “ bulge-dominated ” and n < 2 to be “ disk-dominated ” .
Our n > 2 number fractions at z = 0.1 agree well with those based on Sloan Digital Sky Survey galaxies .
We find that the n > 2 galaxy number fraction is constant with redshift in the field .
However , for overdense environments this fraction is larger and increases towards lower redshifts , higher densities and higher luminosities .
Rest-frame color-magnitude diagrams show that the color distribution is bimodal out to our redshift limit of z \sim 1 with a prominent red-sequence of galaxies at 0.2 < z < 0.4 and a large blue-peak dominance at 0.8 < z < 1 .
We use this bimodality to define a red fraction as the fraction of galaxies having a rest-frame color u ^ { * } - g ^ { \prime } > 1 .
For all environments , this fraction increases towards lower redshifts and higher luminosities .
The red fraction within cluster-like regions changes 60 \% faster with redshift as compared to the field for galaxies with M _ { g ^ { \prime } } < -19.5 .
Using , for the first time , observations across many cluster-field interfaces distributed over a single , large volume , we trace the large-scale morphology-density relation and the Butcher-Oemler effect over a period of almost 8 Gyr .