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Using deep infrared observations conducted with the MOIRCS on the SubaruTelescope in GOODS-N combined with public surveys in GOODS-S, we investigatethe dependence on stellar mass, M_*, and galaxy type of the close pair fraction(5 kpc < r < 20 kpc) and implied merger rate. In common with some recentstudies we find that the fraction of paired systems that could result in majormergers is low (~4%) and does not increase significantly with redshift toz~1.2, with (1+z)^{1.6 \pm 1.6}. Our key finding is that massive galaxies withM_* > 1E11 Msun are more likely to host merging companions than less massivesystems (M_* ~ 1E10 Msun). We find evidence for a higher pair fraction for red,spheroidal hosts compared to blue, late-type systems, in line with expectationsbased on clustering at small scales. So-called "dry" mergers between early-typegalaxies represent nearly 50% of close pairs with M_* > 3E10 Msun at z~0.5, butless than 30% at z~1. This result can be explained by the increasing abundanceof red, early-type galaxies at these masses. We compare the volumetric mergerrate of galaxies with different masses to mass-dependent trends in galaxyevolution, finding that major mergers cannot fully account for the formation ofspheroidal galaxies since z~1. In terms of mass assembly, major mergerscontribute little to galaxy growth below M_* ~ 3E10 Msun but are moresignificant among galaxies with M_* > 1E11 Msun, 30% of which have undergonemostly dry mergers over the observed redshift range. Overall, the relativelymore rapid coalescence of high mass galaxies mirrors the expected hierarchicalgrowth of halos and is consistent with recent model predictions, even if thedownsizing of star formation and morphological evolution involves additionalphysical processes.

The Greater Impact of Mergers on the Growth of Massive Galaxies: Implications for Mass Assembly and Evolution Since z~1