We present the quantitative rest-frame B morphological evolution and galaxy merger fractions at 0.2 < z < 1.2 as observed by the All-wavelength Extended Groth Strip International Survey ( AEGIS ) .
We use the Gini coefficent and M _ { 20 } to identify major mergers and classify galaxy morphology for a volume-limited sample of 3009 galaxies brighter than 0.4 L _ { B } ^ { * } , assuming pure luminosity evolution of 1.3 M _ { B } per unit redshift .
We find that the merger fraction remains roughly constant at 10 \pm 2 % for 0.2 < z < 1.2 .
The fraction of E/S0/Sa increases from 21 \pm 3 % at z \sim 1.1 to 44 \pm 9 % at z \sim 0.3 , while the fraction of Sb-Ir decreases from 64 \pm 6 % at z \sim 1.1 to 47 \pm 9 % at z \sim 0.3 .
The majority of z < 1.2 Spitzer MIPS 24 \mu m sources with L ( IR ) > 10 ^ { 11 } L _ { \odot } are disk galaxies , and only \sim 15 % are classified as major merger candidates .
Edge-on and dusty disk galaxies ( Sb-Ir ) are almost a third of the red sequence at z \sim 1.1 , while E/S0/Sa make up over 90 % of the red sequence at z \sim 0.3 .
Approximately 2 % of our full sample are red mergers .
We conclude ( 1 ) the merger rate does not evolve strongly between 0.2 < z < 1.2 ; ( 2 ) the decrease in the volume-averaged star-formation rate density since z \sim 1 is a result of declining star-formation in disk galaxies rather than a disappearing population of major mergers ; ( 3 ) the build-up of the red sequence at z < 1 can be explained by a doubling in the number of spheroidal galaxies since z \sim 1.2 .